ASTEROID LIGHTCURVE DATABASE (LCDB) EXTENDED NOTES
GENERATED: Oct 01, 2023

ASTEROID LIGHTCURVE DATABASE (LCDB) EXTENDED NOTES
GENERATED: Oct 01, 2023

      1 Ceres                         
        Drummond 2014                  D_equatorial: 967 ± 10 km; D_polar: 892 ± 10 km.

        AKARI                          This note applies to all 'AKARI' details records. The Usui
                                       (2011) paper (AKARI/IRC Survey) used H values from Lowell
                                       Observatory's ASTORB file and assumed ± 0.05 mag error. In
                                       some cases, using the stated values for albedo and diameter
                                       in the standard formulae to compute H (see LCDB README) does
                                       not give the ASTORB value of H, usually differing by
                                       0.01-0.02 mag.


      2 Pallas                        
        Carry 2010a                    Density = 3.4 ± 0.9 g/cc.  Dimensions: a = 275 ± 4 km; b =
                                       258 ± 3 km; c = 238 ± 3 km.

        Durech 2011a                   This applies to all entries for Durech 2011a. All but 14 of
                                       the spin axis values in Durech 2011a are assumed values taken
                                       from the literature. See the original paper for specifics.

        Hanus 2017b                    Hanus 2017b is based on combining photometric, adaptive
                                       optics, and occulation observations.


      3 Juno                          
        Pravec 2012b                   This note applies to all Pravec 2012b entries. In almost all
                                       cases, the original Pravec values were H_R. The H_V values
                                       were derived using assumed V-R values from various sources
                                       based on known taxonomic class or orbital position. If a
                                       diameter and albedo are given, these are revised values based
                                       on the original WISE H, G, D, and pV, corrected using the new
                                       H-G values and Harris and Harris (1997).

        Pal 2020                       This applies to all records from Pal 2019 Period and
                                       amplitude errors were not included in the original data set.
                                       During the mass import of their results table, the period
                                       error was set to five units of the last decimal place. The
                                       amplitude error was set to 20% of the reported amplitude. The
                                       errors are a general guide only and should not be considered
                                       valid for statisitcal studies unless after reviewing the
                                       original plots. These are available at:
                                       http://archive.konkoly.hu/pub/tssys/dr1/object_plots/


      4 Vesta                         
        Fornasier 2011b                Observations made from Rosetta spacecraft.

        Hasegawa 2014b                 H_B: 3.96 ± 0.01, G_B: 0.30 ± 0.02; H_SZ: 3.08 ± 0.02, G_SZ:
                                       0.25 ± 0.01.


      5 Astraea                       
        Durech 2009                    The pole (126, +40) agrees well with occultation profiles.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


      6 Hebe                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Marsset 2017                   Marsset 2017 combined photometric, adaptive optics, and
                                       occultation data.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


      7 Iris                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


      8 Flora                         
        Torppa 2003                    The sidereal period is believed incorrect (see Durech entry
                                       from DAMIT web site). The pole solution is still in close
                                       agreement with other solutions.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless


      9 Metis                         
        Durech 2011web                 Pole solution verified by Keck AO and occulation
                                       observations.

        Drummond 2012                  Effective diameter derived from ellipsoid of 218x175x129 km.


     10 Hygiea                        
        Durech 2011a                   Second pole solution (312,-42) gives a diameter of 443 ± 45
                                       km. This is not the preferred solution.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     11 Parthenope                    
        Mahlke 2021                    The errors for H, G1, G2 are the larger of the HDI 95% values
                                       given for each parameter. In many cases, there are two
                                       entries for each asteroid, one for the c(yan) and the other
                                       for the o(range) ATLAS filter. The taxonomic class is on the
                                       Bus-DeMeo system was taken from various references. This work
                                       did not determine class independently.


     13 Egeria                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Masiero 2017                   The albedo error given for Masiero 2017 is the maximum
                                       possible value when converting from albedo values from log
                                       space to value space.


     14 Irene                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless

        Martikainen 2021               This applies to all Martikainen 2021 entries (A 649, A98). Of
                                       the 492 asteroids in their tables, only 312 were included in
                                       the LCDB: those where H_G, G1, and G2 were found. They found
                                       that H_G and H_V had a strong 1:1 correlation, i.e., in
                                       almost all cases, the two values were essentially the same.
                                       For the Details records, the taxonomic class given by
                                       Martikainen et al. has a suffix of '(T)' (Tholen) or '(BDM)'
                                       Bus-DeMeo. The phase angle is the average of the min/max
                                       phase angles. The PAB values could not be computed. No errors
                                       were given for G1/G2. They have been assumed to be 0.05.
                                       Since the results are based in part on dense lightcurves, the
                                       Survey flag was set to LCI-D even though sparse Gaia data
                                       were included.


     15 Eunomia                       
        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     16 Psyche                        
        Durech 2011a                   Second pole solution (213,1) has a slightly larger error bar
                                       (36 km) for the diameter.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     17 Thetis                        
        Behrend 2007web                Originally reported P = 12.27 ± 0.05. Updated in 2011.

        Behrend 2011web                Originally reported P = 12.259 ± 0.007 h. Updated in 2011
                                       with additional data.


     19 Fortuna                       
        Durech 2011web                 Pole confirmed by HST and occultation observations.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Veres 2015                     Veres et al. (2015) from Pan-STARRS photometry. The value for
                                       G is G12, not G1, and so the G2 values are NULL.


     21 Lutetia                       
        Belskaya 2010a                 The period given was adopted from work by Faury (2008).

        Carry 2010b                    Shape model is non-convex.

        Durech 2017                    Durech 2017: Combined photometric and thermal data.


     22 Kalliope                      
        Descamps 2008a                 Linus D = 28 ± 2 km. Kalliope a = 117.5, b = 82, c = 62 km.

        Marchis 2008c                  D(Linus) > 22 km

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Stephens 2022c                 Based on data set that combined two observing runs about 10
                                       days apart.


     23 Thalia                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     27 Euterpe                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     28 Bellona                       
        Behrend 2006web                Originally reported as 16.3 h.

        Behrend 2007web                Originally reported as 16.32 h.

        Behrend 2008web                Originally reported as 16.623 h. Modified to fit period found
                                       with 2012 data.

        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     29 Amphitrite                    
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     30 Urania                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     31 Euphrosyne                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     32 Pomona                        
        Behrend 2008web                Originally reported with P = 7.1. Updated in 2011 to fit
                                       period found with 2011 data (11.7 h). Updated in 2016 to fit
                                       period found from 2016 data.

        Behrend 2011web                Originally reported P = 7.1 h. Updated in 2011 to fit period
                                       found from 2011 data. Updated in 2016 to force fit to period
                                       found from 2016 data.

        Behrend 2012web                Originally reported 11.7 h. Changed to force a fit to period
                                       found from 2016 data.


     34 Circe                         
        Durech 2011a                   Second pole (275,51) gives a diameter of 107 ± 10 km. The two
                                       solutions are about equally likely.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     35 Leukothea                     
        Pilcher 2009d                  Pole solution was determined using 'amplitude-aspect' method.


     36 Atalante                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     37 Fides                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     39 Laetitia                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     40 Harmonia                      
        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     41 Daphne                        
        Conrad 2008b                   Discovey of S/2008 (41) 1.

        Matter 2011                    The diameter is based on a non-convex model using lightcurves
                                       and AO images. A convex model gives an effective diameter of
                                       194-209 km.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     42 Isis                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     45 Eugenia                       
        Merline 1999                   Discovery of S/1998 (45) 1

        Marchis 2006c                  Detection of known satellite.

        Marchis 2007                   Discovery of second satellite. D ~ 6 km.

        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     47 Aglaja                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     50 Virginia                      
        Fornasier 2011a                The taxonomic classes given by Fornasier et al. are on the
                                       Tholen system.


     52 Europa                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Merline 2013a                  Diameter and albedo based on a rocky body. An equally likely
                                       solution assuming a collection of bare rock slabs gives D =
                                       0.004 ± 0.001 km and pV = 0.45 ± 0.35.


     53 Kalypso                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     54 Alexandra                     
        Torppa 2008a                   Sidereal period is for (307,  20) solution.

        Durech 2011a                   The second pole solution (156,13) is the least preferred. It
                                       also gives a different diameter of 135 ± 20 km and sidereal
                                       period of 7.022641 h.

        Durech 2011web                 The pole solution (318, +23) has P_sidereal = 7.022649 h.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     62 Erato                         
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)

        Jiang 2021                     This note applies to all Jiang 2021 entries. The diameter
                                       error is the larger of a two, non-linear error values.


     68 Leto                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     69 Hesperia                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     70 Panopaea                      
        Wilawer 2022                   This applies to all Wilawer 2022 (MNRAS 513, 3242-3251): The
                                       observations for each asteroid spanned several months. The
                                       phase and PAB angles are for the first date of the
                                       observations (Zero phase). Period errors were not given and
                                       so assumed to be 2 units of the last decimal place.


     72 Feronia                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     80 Sappho                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     81 Terpsichore                   
        Timerson 2010                  The diameter was calculated from the a/b values for the
                                       best-fit ellipse. It represents a minimum value.

        Timerson 2010                  The diameter was calculated from the a/b values for the
                                       best-fit ellipse. It represents a minimum value.


     82 Alkmene                       
        Timerson 2015                  Occultation profile gives ellipsoid of 62.8 ± 0.9 x 55.4 ±
                                       0.9 km. Effecitve diameter is based on area of the ellipse.
                                       The shape supports model 146 on the DAMIT site
                                       (http://astro.troja.mff.cuni.cz/projects/asteroids3D/web.php)
                                       


     83 Beatrix                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     85 Io                            
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     87 Sylvia                        
        Behrend 2012web                Single lightcurve from data spanning two months. The
                                       amplitude, and possibly synodic period, seemed to have
                                       changed over the interval.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Carry 2021                     Multiple lightcurves from 1978-08-30 to 2008-04-01.


     88 Thisbe                        
        Durech 2011a                   The second pole solution (247,50) gives a slightly larger
                                       effective diameter: 220 ± 16 km. This is the least preferred
                                       solution.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     89 Julia                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     90 Antiope                       
        Merline 2000a                  Discovery of satellite.

        Bartczak 2014                  D1: 80.8 ± 1.8 km. D2: 80.4 ± 1.8 km. Separation: 174 ± 4 km.


     93 Minerva                       
        Torppa 2008a                   Sidereal period is for (49, -40) pole solution.

        Marchis 2009                   Estimated sizes: S1 4km; S2 3 km.

        Behrend 2011web                Originally reported as P = 5.98 ± 0.05 h. Forced in 2012 to
                                       agree with period found using 2012 data.

        Marchis 2011a                  D_MinervaI = 4 ± 2 km. D_MinervaII = 3 ± 1 km. P_Orb(MI) =
                                       57.79 h. P_Orb(MII) = 26.74 h.


     94 Aurora                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     97 Klotho                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     99 Dike                          
        Waszczak 2015                  Waszczak (2016) H values are based on G12 system. The G12
                                       value is given instead of G and carries 'G' for the source
                                       flag. The LCDB U value is based on the Waszczak et al.
                                       'relflag' value, with relflag = 0 given U = 1 and relflag = 1
                                       given U = 2


    103 Hera                          
        Wang 2019                      G2: 0.45(1)


    105 Artemis                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    107 Camilla                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Marsset 2016                   Discovery of second satellite.

        Pajuelo 2018a                  Orbital period in binaries table is for S1. S2


    108 Hecuba                        
        Behrend 2005web                Originally reported 19.8 h. Updated in 2016 to fit new
                                       period.


    114 Kassandra                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    119 Althaea                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    121 Hermione                      
        Descamps 2009a                 Pole (4, +13) has P_sidereal = 5.550878 h and is based on
                                       non-convex model.


    125 Liberatrix                    
        Durech 2007                    The pole (280, +74) has P_sidereal = 3.968199 h.


    126 Velleda                       
        Behrend 2011web                Originally reported P = 5.36 ± 0.05 h, A = 0.05 ± 0.01 mag.
                                       Updated in 2011 after additional data obtained.


    128 Nemesis                       
        Doubled period (~78 h) cannot be formally excluded.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    129 Antigone                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    130 Elektra                       
        Behrend 2001web                Originally reported P = 5.43 h. Data forced to fit period
                                       found in 2011.

        Behrend 2009web                Period originally reported as 5.43 ± 0.01 h.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Yang 2014                      S/2014 (130) 1. Second satellite. Projected separation from
                                       primary approx. 550 km.

        Berdeu 2021                    Discovery of third satellite.


    132 Aethra                        
        Binzel 2019                    MITHNEOS Method: VISNIR This note applies to all Binzel 2019
                                       (2019Icar..324...41B) detail records:  For the MITHNEOS
                                       method,  VIS indicates visible data only.  NIR indicates
                                       near-infrared data only.  VISNIR indicates both. eVISNIR
                                       indicates the visible portion of the spectrum is from the
                                       Eight-Color Asteroid Survey (ECAS, Zellner et al. 1985) sVis
                                       indicates the visible portion of the spectrum is from the
                                       Sloan Digital Sky Survey (SDSS, Ivezic et al. 2001). TAXON
                                       indicates the type is reported in the literature; see the
                                       source listed in the 'Taxon' reference column of the original
                                       file.  For visible data only (VIS), the taxonomic type is
                                       from the Bus classification system (Bus and Binzel 2002). For
                                       visible plus near-infrared data (VISNIR), the taxonomic type
                                       is from the Bus-DeMeo classification system (DeMeo et al.
                                       2009).  '-comp' refers to the broad taxonomic complex. When
                                       multiple taxonomic classes are listed, they are in subjective
                                       order of most likely type first. ':' indicates the assignment
                                       is


    135 Hertha                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    136 Austria                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Durech 2016                    Models from Durech et al. (2016) are posted on the DAMIT web
                                       site.
                                       http://astro.troja.mff.cuni.cz/projects/asteroids3D/web.php


    139 Juewa                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    145 Adeona                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Wang 2018                      Sidereal period for pole (122, -3): 15.0733 h


    146 Lucina                        
        Durech 2009                    The pole (305, -41) has P_sidereal = 18.55390 h.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    152 Atala                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    153 Hilda                         
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html

        Warner 2021i                   Model axis ratios (c = 1.0): a/b = 1.14, a/c = 1.4839.


    155 Scylla                        
        Hanus 2018b                    The Hanus 2018b entries include results only if they are
                                       revisions or rejections of previously reported pole
                                       solutions.


    158 Koronis                       
        Erasmus 2020                   This note applies to all Erasmus 2020 (2020ApJS..247...13E)
                                       detail records: Initial bulk data entry assigned U = 2 for a
                                       period probability >= 75 and U = 2- for < 75. The family
                                       class (C or S) was assigned based on which had the higher
                                       probability (if 50, CS was assigned). All family values of
                                       Nysa-Polana were assigned to Nysa family. SWF (Sparse
                                       Wide-field) was assigned to the Survey entry.


    160 Una                           
        Marciniak 2009a                Pole (308, -41) has P_sidereal = 11.03316 h.


    161 Athor                         
        Pilcher 2010b                  Pole solution was determined using 'amplitude-aspect' method.


    165 Loreley                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    167 Urda                          
        Durech 2011a                   The second pole solution (107,-69) gives a slightly larger
                                       effective diameter: 51 ± 15 km. This is the least preferred
                                       solution.


    176 Iduna                         
        Wang 2018                      Sideral period for pole solution (156,+73): 11.29382 h.


    178 Belisana                      
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)


    184 Dejopeja                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    194 Prokne                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    196 Philomela                     
        Durech 2007                    Pole (276, -49) has P_sidereal = 8.332827 h.


    198 Ampella                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    201 Penelope                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    202 Chryseis                      
        Behrend 2005web                Originally reported P = 11.8 ± 0.5. Updated in 2011.


    208 Lacrimosa                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    211 Isolda                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    216 Kleopatra                     
        Marchis 2008e                  AO observations show two satellites, ~5 km and ~3 km.
                                       Distances: 650 km and 380 km, respectively.

        Shepard 2018                   DimensionsL 276 x 94 x 178 km


    221 Eos                           
        Hanus 2018a                    Hanus 2018 combined optical photometric and IR (WISE) data
                                       for shape modeling. Shape modeling quality rating (QF) is
                                       from Hanus 2017c.


    224 Oceana                        
        Behrend 2006web                Originally reported P = 18.93 ± 0.05. Updated in 2011.


    228 Agathe                        
        Szabo 2016                     The plots for Szabo 2016a were made available off-line. They
                                       were not included in the original paper or in supplemental
                                       data.


    230 Athamantis                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    238 Hypatia                       
        Behrend 2004web                Originally reported 8.88 h. Updated in 2011.


    239 Adrastea                      
        Behrend 2007web                Originally reported as 19.846 h. Modified based on results
                                       from later observations.


    250 Bettina                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    266 Aline                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    271 Penthesilea                   
        Podlewska-Gaca 2021            This note applies to all Podlewska-Gaca et al. (2021) Ap. J.
                                       Suppl. Ser. 2021, id. 4. The given observation date is the
                                       mid-date for runs C9a and C9b. Few lightcurves were
                                       published. By default, entries from Table 2 were assigned U =
                                       2; entries from Table 3 were rated U = 2-. entries in Table 4
                                       were also given U = 2- with the errors assumed to be 25% of
                                       the listed period.


    275 Sapientia                     
        Dose 2022c                     G values in Dose 2022c were derived by finding the value for
                                       G that gave the lowest RMS fit to the Fourier curve. The
                                       value for G may or may not be consistent with the taxonomic
                                       classification.


    276 Adelheid                      
        Durech 2011a                   The second pole solution (199,-20) gives a slightly smaller
                                       diameter: 117 ± 15 km. The two solutions are about equally
                                       likely.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.
                                       Occultation-inversion gives D = 125 ± 15.


    282 Clorinde                      
        Dose 2023a                     The values for G in Dose 2023 (MPB 50, 65-73) were found by
                                       minimizing the RMS scatter of a Fourier fit, not by strict
                                       calculation.


    283 Emma                          
        Durech 2011web                 Pole (251, +22) has P_sidereal = 6.895222 h.


    298 Baptistina                    
        Carvano 2010                   H_R = 10.92 was directly measured value. The H = 11.30 is the
                                       result of using H_R and V-R = 0.38 measured by the authors.


    302 Clarissa                      
        Durech 2011a                   The first pole solution (28,-72) is preferred.


    306 Unitas                        
        Durech 2011a                   The second pole solution (253,-17) gives a slightly larger
                                       diameter: 53 ± 5. This is the least preferred solution.


    308 Polyxo                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    312 Pierretta                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    317 Roxane                        
        Merline 2009                   Estimated Ds/Dp: 0.26 (based on magnitude differences).


    331 Etheridgea                    
        Warner 2010i                   Presuming the nightly calibrations were correct, the data
                                       provide any number of solutions. If the two sessions are
                                       forced to overlay, a number of solutions, less than 24 h, are
                                       still possible.


    345 Tercidina                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    349 Dembowska                     
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    350 Ornamenta                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    352 Gisela                        
        Erasmus 2020                   This note applies to all Erasmus 2020 (2020ApJS..247...13E)
                                       detail records: Initial bulk data entry assigned U = 2 for a
                                       period probability >= 75 and U = 2- for < 75. The family
                                       class (C or S) was assigned based on which had the higher
                                       probability (if 50, CS was assigned). All family values of
                                       Nysa-Polana were assigned to Nysa family. SWF (Sparse
                                       Wide-field) was assigned to the Survey entry.


    354 Eleonora                      
        Behrend 2001web                Originally reported P = 4.3 ± 0.1. Updated in 2011 to fit
                                       data to a period found with a different data set.

        Behrend 2002web                Originally reported P = 4.282 ± 0.005, A = 0.52 ± 0.02.
                                       Updated in 2011.

        Behrend 2006web                Originally reported P  = 4.27750 ± 0.00003 h, A = 0.20 ±
                                       0.01. Updated in 2011.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    355 Gabriella                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    362 Havnia                        
        Wang 2015b                     Period for second pole is 16.918935 ± 0.000043 h.


    370 Modestia                      
        Athanasopoulos 2022            The orginal paper reported a pole of (268, -92).  |Latitude|
                                       > 90 deg is not allowed in LCDB. In such a case, 180 deg is
                                       added to or subtracted from the longitude and the
                                       complimentary latitude is used. In this case, that means
                                       latitude = -88 deg.


    372 Palma                         
        Durech 2011a                   The second pole solution (44,17) gives a different diameter
                                       (198 ± 26 km) and sidereal period (8.58191 h). The two
                                       solutions are about as likely.


    374 Burgundia                     
        Behrend 2018web                Two halves of 13-h period are identical, leaving half-period
                                       a distinct possibility.


    382 Dodona                        
        Behrend 2021web                The two earliest observation runs were ignored in assigning
                                       the U code. They are what appear to be obvious outliers.


    386 Siegena                       
        Behrend 2004web                Period originally reported as 7.6 h.


    390 Alma                          
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    391 Ingeborg                      
        Binzel 2019                    MITHNEOS Method: VIS


    394 Arduina                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    409 Aspasia                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.
                                       Occultation-inversion gives D = 173 ± 17 km.


    414 Liriope                       
        Chang 2015                     Chang (2015) H values are based on H-G system. The G values
                                       are in R, not V. All lightcurves rated U=2-3 by Chang were
                                       reviewed and a formal U code was assigned by the LCDB
                                       authors. The objects in their U = 1 list were all given U =
                                       1.


    418 Alemannia                     
        Gorby 2018                     Results table has incorrect period.


    423 Diotima                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    433 Eros                          
        Trilling 2010                  The Trilling (2010) results are based on using values for H
                                       taken from the JPL Horizons site. In Trilling (2010), there
                                       is often a significant disagreement among the albedo,
                                       diameter, and H values when they are applied to the standard
                                       formula that relates these three values (see LCDB README
                                       file), i.e., using the Trilling albedo and diameter values
                                       gives a differnt value for H than stated, sometimes by up to
                                       0.1 mag.

        Mueller 2011a                  H and G taken from other sources.

        Thomas 2011b                   This note applies to all entries for Thomas 2011b. Warm
                                       Spitzer observations. The error is the larger of the + or -
                                       (which were not the same).

        Binzel 2019                    MITHNEOS Method: VISNIR


    434 Hungaria                      
        Morrison 1979                  Morrison values were based on V(1,0) magnitude system. They
                                       have been converte

        Lucas 2017                     The Lucas 2017 taxonomic classifications are on the Bus-DeMeo
                                       system.

        Wang 2021                      This applies to all Wang & Xu (2021). The pole coordinates
                                       and sidereal period uncertanties were not specified. Default
                                       errors for longitude and latitude of ± 10 deg were used while
                                       the default period error used was 2 units in the last decimal
                                       place.


    435 Ella                          
        Chang 2016                     Chang (2016) H values are based on H-G system. The G values
                                       are in R, not V. All lightcurves with a period were initially
                                       given U = 2 regardless of rating by Chang et al. The plots
                                       for the 352 lightcurves that did not have complete coverage
                                       were reviewed and the U codes revised. In many of those
                                       cases, it appears that the half-period was found. For those,
                                       if the summary line depended on the Chang et al. entry, the
                                       period on the summary line is double that found by Chang et
                                       al. and carries a 'D' (determined) flag in the NOTES field.
                                       No errors were given for amplitudes, which were often
                                       dramatically overstated.


    437 Rhodia                        
        Behrend 2005web                Originally reported 52.8 h. Updated to fit period found with
                                       2016 data.


    444 Gyptis                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    469 Argentina                     
        Wang 2003                      BIN: Reported possibility of being binary.      Considered
                                       unreliable.

        Wang 2005                      NPA: Reported secondary period of 8.74 hr.       Considered
                                       unreliable.


    470 Kilia                         
        Pilcher 2020f                  Second period of 119.3 h in lc_npar is one of several
                                       possibilities.


    471 Papagena                      
        Torppa 2008a                   Sidereal period is for (29, 41) solution.


    475 Ocllo                         
        Binzel 2019                    MITHNEOS Method: TAXON


    479 Caprera                       
        Behrend 2002web                Originally reported P = 5.259 ± 0.002 h, A = 0.34 ± 0.09 h.
                                       Updated in 2011 to fit data to a new period found with a
                                       different data set.

        Behrend 2004web                Originally reported P = 5.247 ± 0.006 h, A = 0.08 ± 0.01 mag.
                                       Updated in 2011 to fit to a new period found from a different
                                       data set.

        Behrend 2007web                Originally reported P = 5.2491 ± 0.0002, A = 0.07 ± 0.01 mag.
                                       Updated in 2011 to fit data a new period found with a
                                       different data set.


    488 Kreusa                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    506 Marion                        
        Wang 2015b                     Period for second pole solution is 16.549751 ± 0.000060


    511 Davida                        
        Conrad 2007                    Measured ellipsoid (a,b,c): 357±2, 294±2, 231±50 km.


    512 Taurinensis                   
        Binzel 2019                    MITHNEOS Method: VISNIR


    522 Helga                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    531 Zerlina                       
        Behrend 2002web                Originally reported 7.2 h. Updated to fit period found with
                                       2016 data.


    540 Rosamunde                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    544 Jetta                         
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    550 Senta                         
        Behrend 2004web                Originally reported 19.584 h. Updated to fit period found in
                                       2016.

        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    566 Stereoskopia                  
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    585 Bilkis                        
        Wang 2016                      All lightcurves for Wang et al. 2016 were forced to sidereal
                                       period and were in intensity units of the inversion model
                                       curve, therefore there were no amplitudes in magnitude given.
                                       


    588 Achilles                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


    617 Patroclus                     
        Buie 2015                      Volume equivalent diameters based on derived ellipsods are
                                       D_Patroclus: 113 km; D_Menoetius: 104 km

        Chatelain 2016                 The B-V and V-R magnitudes for the Chatelain 2016 (Icarus
                                       271) were derived from the data table in Appendix A. The
                                       median errors for these color indexes in the paper are given,
                                       not the actual values for the individual results. The B-R and
                                       V-I magnitudes are from Table 3. The B-V and V-R values may
                                       not yield the exact numbers of the stated B-R and V-I
                                       magnitudes.

        Berthier 2020                  Area-equivalent diameter.


    624 Hektor                        
        The objects under Sonnett 2015 were observed in the W3 (12 um) band by WISE. The amplitude
        given is the maximum range of values, not the range of a fitted lightcurve. No periods were
        given for the data.


    636 Erika                         
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    654 Zelinda                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    676 Melitta                       
        Behrend 2002web                Originally reported as 8.5734.

        Behrend 2006web                Originally reported as 14.09 h.


    694 Ekard                         
        Timerson 2010                  A least squares fit to the irregular shape derived from the
                                       occultation observations and based on a shape model by Torppa
                                       et al. (2003) yields the stated diameter.

        Timerson 2010                  A least squares fit to the irregular shape derived from the
                                       occultation observations and based on a shape model by Torppa
                                       et al. (2003) yields the stated diameter.


    699 Hela                          
        Behrend 2003web                Originally reported 4.765 h. Updated to fit period found with
                                       2016 data.

        Binzel 2019                    MITHNEOS Method: VISNIR


    702 Alauda                        
        Rojo 2011                      R_orbit = 1230 km.


    704 Interamnia                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    719 Albert                        
        Binzel 2019                    MITHNEOS Method: VISNIR


    727 Nipponia                      
        Baxter 2019                    Baxter et al. (2019) also reported shape models for each
                                       asteroid in their paper, but did not give the sidereal period
                                       or pole solution.


    728 Leonisis                      
        Galad 2010c                    The lightcurves from Galad 2010c are based on data from the
                                       SDSS Moving Object Catalog.


    763 Cupido                        
        Pilcher 2018d                  Ambiguous second period. Other possibility is 121 h.


    777 Gutemberga                    
        Polakis 2018d                  The ambiuous table includes the half-period for this work.
                                       However, given the amplitude and low phase angle, the LCDB
                                       authors chose not to include the 'A' flag in the Notes field
                                       of this record or the summary line.


    786 Bredichina                    
        Dose 2021b                     The period/amplitude given in results table are significantly
                                       different from those in the plot. The latter were close to
                                       previous results and so adopted for this entry.


    809 Lundia                        
        Marchis 2012                   Hv assumed V-R = 0.54.

        Bartczak 2017                  Reported pole is the pole of the orbit for the fully
                                       syncrhonous binary. Amplitudes are for out of eclipse
                                       lightcurve.


    825 Tanina                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    853 Nansenia                      
        Behrend 2001web                Originally reported P = 9.31 h. Update in 2011 based on a new
                                       period but the solution is still highly ambiguous.


    854 Frostia                       
        Marchis 2012                   Hv assumed V-R = 0.54.


    887 Alinda                        
        Morrison 1974                  Morrison gives D = 5. in his table as well as log(D). The
                                       latter results in a value of 5.2 km. We used the latter.

        Dunlap 1979                    The authors give H_v(1,0) = 14.10 ± 0.08. For conversion to
                                       the current H-G system, we use Ho = H(1,0) - 0.34.

        Binzel 2019                    MITHNEOS Method: eVISNIR

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


    901 Brunsia                       
        Wisniewski 1997                A period of 3.139 h (with bimodal curve) was also found by
                                       Wisniewski but the final paper adopted the triply-periodic
                                       value of 4.872 h.


    911 Agamemnon                     
        Timerson 2013                  Ds = 3-10 km. Based on single video observation.


    925 Alphonsina                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    939 Isberga                       
        Carry 2015                     D1: 12.4 ± 2.5 km; Ds: 3.6 ± 0.7 km


    951 Gaspra                        
        Thomas 1994                    Diameter is mean radius of irregular object with principal
                                       diam

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    966 Muschi                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    987 Wallia                        
        Behrend 2008web                Period originally reported as 7.0 h.


   1011 Laodamia                      
        Apostolovska 2014              a/b: 0.83; b/c: 1.3

        Binzel 2019                    MITHNEOS Method: VISNIR


   1016 Anitra                        
        Pilcher 2016f                  Orbital period an approximate estimate based on four possible
                                       mutual events. First entry (Date: Nov 8, 2015) is for full
                                       data set covering three months. Subsequent entries are based
                                       on subsets.


   1036 Ganymed                       
        Velichko 2012                  Obs date estimated from phase angle given in paper.

        Velichko 2013                  Ellipsoid lengths: a = 960 km, b = 770 km, c = 495 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1052 Belgica                       
        Franco 2013b                   Ds/Dp >= 0.36 ± 0.02

        Franco 2013c                   Ds/Dp = 0.36 ± 0.02

        Franco 2020e                   The original paper gives Ds/Dp > 0.34. The 0.16 mag
                                       attenuation gives closer to 0.39. The latter is given in the
                                       lc_binaries table.


   1055 Tynka                         
        Behrend 2012web                Originally reported as P = 12.8 ± 0.5 h.

        Fornas 2023a                   Stepehens data (ALCDEF, 2012 Mar-May) included for analysis.


   1061 Paeonia                       
        Pilcher 1987                   Pilcher's notes for 1986 Dec. 4 show observations form
                                       4:20-8:00 UT with fading by about 0.5 magnitude 5:10-7:00 UT,
                                       then brightening by 8:00.  For 1986 Dec. 5, 1061 Paeonia was
                                       'fairly easy at 5:20, 6:15, invisible at 7:20, dimly seen
                                       again 8:05 at lower altitude.


   1065 Amundsenia                    
        Binzel 2019                    MITHNEOS Method: VIS


   1069 Planckia                      
        Behrend 2006web                Originally reported P = 11. h, A = 0.18. Updated in 2011 to
                                       fit data to new period.


   1070 Tunica                        
        Waszczak (2015) H values are based on G12 system. The G12 value is given instead of G and
        carries 'G' for the source flag. The G2 value is NUL. The LCDB U value is based on the
        Waszczak et al. 'relflag' value, with relflag = 0 given U = 1 and relflag = 1 given U = 2


   1082 Pirola                        
        Baker 2011a                    When using maximum light, H = 10.320 ± 0.013, G = 0.107 ±
                                       0.016.


   1089 Tama                          
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Behrend 2011web                Originally reported P = 16.45 ± 0.05, A = 0.12 ± 0.02 mag.
                                       Updated in 2011 with additional data.


   1095 Tulipa                        
        Behrend 2005web                Originally reported P = 2.78730 ± 0.00005 h, A = 0.20 ± 0.01
                                       mag. Updated in 2011.


   1100 Arnica                        
        Slivan 2008                    A footnote to Table 2 in the Slivan et al. (2008) paper
                                       indicates that subsquent data (not included in the paper)
                                       show the period to be 14.535 h instead of the ~29 h reported
                                       in the paper. The 2007 data were not plotted in the paper.


   1131 Porzia                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1134 Kepler                        
        Binzel 2019                    MITHNEOS Method: VIS


   1139 Atami                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1152 Pawona                        
        Wang 2022                      Sidereal period for (162, 58) and (323, 61): 3.41437 h.


   1170 Siva                          
        Binzel 2019                    MITHNEOS Method: TAXON


   1183 Jutta                         
        Erasmus 2021                   This note applies to all Erasmus et al. (2021, MNRAS). The Hv
                                       from JPL is generally within Â±0.3 mag of the ATLAS H_c
                                       values reported in the paper. The C/S taxonomic class is
                                       dervived from the color indices and express as a probability.
                                       For the LCDB entries, objects >= 66% of C or S are assigned a
                                       single letter. Otherwise, C/S is listed.


   1188 Gothlandia                    
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Baker 2012a                    Using maximums of lightcurves, the authors found H = 11.425 ±
                                       0.014 and G = 0.230 ± 0.015. Diameter and albedo are
                                       revisions to WISE values applying the author's H-G and Harris
                                       and Harris (1997) correction.


   1198 Atlantis                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1204 Renzia                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1207 Ostenia                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1268 Libya                         
        Warner 2023e                   Primary period (14.11) not ambiguous but there is a secondary
                                       period of 5.04 h that improves the primary lightcurve fit
                                       considerably but may not have a physical cause.


   1270 Datura                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1278 Kenya                         
        Oey 2012b                      The second tumbling period of 127 h is a likely but not
                                       definitive candidate.


   1293 Sonja                         
        Binzel 2019                    MITHNEOS Method: VIS


   1310 Villigera                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


   1313 Berna                         
        Marchis 2012                   Hv assumed V-R = 0.54.


   1316 Kasan                         
        Binzel 2019                    MITHNEOS Method: VIS


   1333 Cevenola                      
        Marchis 2012                   Hv assumed V-R = 0.54.


   1346 Gotha                         
        Behrend 2006web                Originally reported P = 2.6540 ± 0.0003 h.


   1374 Isora                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1406 Komppa                        
        Behrend 2011web                Authors reported P = 7.02 with 4 max/min.


   1428 Mombasa                       
        Stephens 2012web               A half-period of 8.38 h cannot be formally excluded.


   1443 Ruppina                       
        Stephens 2020e                 axis ratios (c=1): a/b: 1.291, a/c: 1.210


   1453 Fennia                        
        Warner 2016i                   To find the primary period, the satellite orbital period was
                                       forced to near previous results.


   1468 Zomba                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1474 Beira                         
        Binzel 2019                    MITHNEOS Method: TAXON


   1489 Attila                        
        Chang 2019a                    This note applies to all Chang 2019 (ArXiv:1901.08719) detail
                                       records: The U code reported in Chang et al. is not
                                       necessarily the LCD value. Initial bulk data entry assigned U
                                       = 2 pending individual review. Amplitude errors were not
                                       given. A default of 10% of the amplitude was assigned pending
                                       individual review


   1499 Pori                          
        Behrend 2008web                Originally 3.36 h. Updated to fit period found in 2016.


   1508 Kemi                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1509 Esclangona                    
        Merline 2003a                  Ds ~4 km. Distance from Primary: 140 km.

        Marchis 2012                   Hv assumed V-R = 0.54.


   1512 Oulu                          
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   1514 Ricouxa                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1536 Pielinen                      
        Casalnuovo 2016                Secondary period P = 6.43 ± 0.01 h reported. Likely harmonic
                                       of main period.


   1565 Lemaitre                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1566 Icarus                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1580 Betulia                       
        Binzel 2019                    MITHNEOS Method: sVISNIR


   1593 Fagnes                        
        Binzel 2019                    MITHNEOS Method: VIS


   1620 Geographos                    
        Durech 2008b                   Pole/period in spin axis table are for 1969 January 7.5. YORP
                                       acceleration found.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Durech 2022                    YORP parameter: 1.14(03)*(10^-8 rad d^-2)


   1627 Ivar                          
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1640 Nemo                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1656 Suomi                         
        Franco 2022d                   Unexplained attenuation on 2022 May 18.


   1667 Pels                          
        Stephens 2020e                 axis ratios (c=1): a/b:1.247m a/c: 1.135


   1685 Toro                          
        Binzel 2019                    MITHNEOS Method: VISNIR

        Durech 2022                    YORP Parameter: 0.33(3) * (10^-8 rad d^-2)


   1723 Klemola                       
        Behrend 2005web                Originally reported P = 6.22 h. Updated in 2011 to fit period
                                       found with 2011 data.


   1727 Mette                         
        Behrend 2003web                Period originally reported as 2.982 ± 0.002 h.

        Behrend 2006web                Originally reported as P = 2.98141 ± 0.00005 h.

        Warner 2013i                   Ds/Dp: >= 0.20 ± 0.02. Unusual because primary is moderately
                                       elongated, a/b = 1.36:1 assuming equatorial view of triaxial
                                       ellipsoid.

        Warner 2013l                   Ds/Dp = 0.21 ± 0.02

        Warner 2016l                   Orbital period forced to range near previous results. As
                                       stand-alone data set, insufficient evidence to suggest a
                                       satellite.


   1741 Giclas                        
        Pravec 2019b                   Paired with (258640) 2002 ER36. This note applies to all
                                       Pravec 2019b:  Albedos were not reported. They were
                                       calculated based on the H and Diameter given in the paper.
                                       This was done to allow comparing the albedo required to match
                                       the given values against the albedo given in the summary
                                       and/or other detail records.


   1747 Wright                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1770 Schlesinger                   
        Pravec 2016web                 Orbital periods for 2016 have no real meaning. They were used
                                       to demonstrate behavior of lightcurve data beyond primary
                                       lightcurve. The 2015 secondary period could be independent
                                       rotation of the satellite or signs of a third member.


   1777 Gehrels                       
        Pravec 1990web                 Reanalysis of the Wisniewski data.


   1778 Alfven                        
        Chang 2014a                    This note applies to all entries from Chang et al. (2014, ApJ
                                       788, A17) where they used 2nd order Fourier fits This
                                       produced amplitudes that didn't necessarily fit the data. The
                                       amplitudes in the LCDB were determined by the LCDB authors.
                                       In some cases, the precision of the period was considered too
                                       high and rounded to the nearest 0.1 h while in other cases,
                                       the stated period was converted to a >X h estimate.


   1829 Dawson                        
        Galad 2010c                    Combined with data from Pray (2006a)


   1830 Pogson                        
        Pravec 2012a                   D2/D1 = 0.28 ± 0.02. Value of D2/D1 = 0.30 ± 0.02 was adopted
                                       as mean of data from three apparitions.

        Pravec 2012a                   Asynchronous status assigned to satellite generating mutual
                                       events.

        Fauerbach 2019e                The known secondary period of 3.2626 h was used to extact the
                                       primary rotation period.


   1850 Kohoutek                      
        Chang (2016) H values are based on H-G system. The G values are in R, not V. All lightcurves
        with a period were initially given U = 2 regardless of rating by Chang et al. The plots for
        the 352 lightcurves that did not have complete coverage were reviewed and the U codes
        revised. In many of those cases, it appears that the half-period was found. For those, if
        the summary line depended on the Chang et al. entry, the period on the summary line is
        double that found by Chang et al. and carries a 'D' (determined) flag in the NOTES field. No
        errors were given for amplitudes, which were often dramatically overstated.


   1862 Apollo                        
        Kaasalainen 2007               Period is for zero-epoch of November 13, 1980. Paper proved
                                       spin up due to YORP effect.

        Rozitis 2013                   The authors assumed the pole and sidereal period from
                                       previous works to derive the required diameter and albedo to
                                       fit a thermophysical model that accuratly predicts Yarkovsky
                                       and YORP rates of change.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1863 Antinous                      
        Masiero 2017                   The albedo error given for Masiero 2017 is the maximum
                                       possible value when converting from albedo values from log
                                       space to value space.

        Binzel 2019                    MITHNEOS Method: VIS


   1864 Daedalus                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Masiero 2020a                  This note applies to all entries for Masiero et al. (2020a).
                                       The albedo error is the listed maximum possible value when
                                       converting albedo values from log space to value space. The
                                       phase angle in the details record is from the file since the
                                       actual date of observation was not given. The value for H is
                                       the 'model-out' value, which may differ slightly from the
                                       value used in the NEATM modeling (the value given in Tables
                                       1-4). This maintains full agreement with the listed albedo
                                       and diameter. See Masiero et al. (2020a) for details about
                                       assumed errors in H and G.


   1865 Cerberus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1866 Sisyphus                      
        Benner 1985                    Ds/Dp ~ 0.1

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1876 Napolitania                   
        Warner 2016b                   Suspected wide binary where primary has long period and large
                                       amplitude and the satellite has a short period and low
                                       amplitude.


   1915 Quetzalcoatl                  
        Binzel 2019                    MITHNEOS Method: TAXON


   1916 Boreas                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1917 Cuyo                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1937 Locarno                       
        Behrend 2019web                Reported period 53.6 h but given amplitude and phase, the
                                       double period is more likely.


   1943 Anteros                       
        Mueller 2011a                  H and G taken from other sources.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1947 Iso-Heikkila                  
        Galad 2010c                    For Galad 2010c entries, a compromise date of 2005 Oct 5 was
                                       used to compute phase and PAB for those objects based on SDSS
                                       data where no specific date information was provided.


   1951 Lick                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1979 Sakharov                      
        Pravec 2011web                 Some suspected events seen but there was no consisetent
                                       solution for a secondary period.


   1980 Tezcatlipoca                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   1981 Midas                         
        Binzel 2019                    MITHNEOS Method: VISNIR

        McGlasson 2022                 A shape was reported (4x2x2) with one lobe being 30% larger.
                                       The neck joining the two lobes is about 60% of the width of
                                       the lobes.


   2006 Polonskaya                    
        Pray 2005c                     Second period due to 1) asynchronous single satelltie or 2)
                                       second satellite.


   2020 Ukko                          
        Pilcher 2015i                  Alternation solutions with bimodal and trimodal solutions are
                                       considered unlikely.


   2030 Belyaev                       
        The errors for H, G1, G2 are the larger of the HDI 95% values given for each parameter. In
        many cases, there are two entries for each asteroid, one for the c(yan) and the other for
        the o(range) ATLAS filter. The taxonomic class is on the Bus-DeMeo system was taken from
        various references. This work did not determine class independently.


   2059 Baboquivari                   
        Masiero 2021                   This note applies to all entries for Masiero et al. (2021;
                                       Plan. Sci. J. 2, A162). The albedo error is the listed
                                       maximum possible value when converting albedo values from log
                                       space to value space. The phase angle in the details record
                                       is from the file since the actual date of observation was not
                                       given. The value for H is the 'model-out' value, which may
                                       differ slightly from the value used in the NEATM modeling
                                       (the value given in Tables 1-4). This maintains full
                                       agreement with the listed albedo and diameter. No specific
                                       errors for H and G were given. Default values of H_err = 0.05
                                       and G_err = 0.1 were used.


   2060 Chiron                        
        Belskaya 2010b                 To derive H, used V-R=0.36 and phase coefficient (not G) of
                                       0.06 mag/degree.

        Belskaya 2015                  The Belskaya et al. (2015) provides updated color index
                                       values for TNOs based on numerous references. See that paper
                                       for the original references.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


   2061 Anza                          
        Binzel 2019                    MITHNEOS Method: TAXON


   2062 Aten                          
        Binzel 2019                    MITHNEOS Method: NIR


   2063 Bacchus                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2064 Thomsen                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2074 Shoemaker                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   2077 Kiangsu                       
        Binzel 2019                    MITHNEOS Method: sVIS


   2078 Nanking                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2099 Opik                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   2100 Ra-Shalom                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   2102 Tantalus                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Rozek 2022                     Radar did not detect a satellite D > 75 m, which leaves
                                       earlier reports of a secondary period unexplained.


   2110 Moore-Sitterly                
        Pravec 2019b                   Paired with (44612) 1999 RP27.


   2121 Sevastopol                    
        Sokova 2019                    Orbital period for retrograde solution: 37.153 Ãƒâ€šÃ‚Â±
                                       0.001 h.


   2178 Kazakhstania                  
        Benishek 2018m                 Secondary has lightcurve amplitude of 0.02 mag;


   2201 Oljato                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   2204 Lyyli                         
        Binzel 2019                    MITHNEOS Method: VIS


   2207 Antenor                       
        Stephens 2018k                 Orbital period is Binaries table is one of several solutions.


   2212 Hephaistos                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   2242 Balaton                       
        Marchini 2016b                 Estimated Ds/Dp is a minimum.


   2253 Espinette                     
        Binzel 2019                    MITHNEOS Method: VIS


   2312 Duboshin                      
        Warner 2023e                   P = 51.72 has significant secondary period of P2 = 19.58 h,
                                       A2 = 0.30. The two may be harmonically related (3:8 ratio).


   2320 Blarney                       
        Bennefeld 2009b                The Pal et al. result of 5.99 h is considered highly secure.
                                       The periods are close to a 7:6 ratio and the data from
                                       Bennefield will fit 5.99 h.

        Behrend 2020web                The Pal et al. result of 5.99 h is considered highly secure.
                                       The periods are close to a 14:13 ratio and the data from
                                       Behrend will fit 5.99 h.


   2329 Orthos                        
        Binzel 2019                    MITHNEOS Method: VIS


   2335 James                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   2340 Hathor                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   2343 Siding Spring                 
        Pollock 2015b                  Secondary period in binary report attributed to third body.


   2368 Beltrovata                    
        Binzel 2019                    MITHNEOS Method: TAXON


   2384 Schulhof                      
        Vokrouhlicky 2016b             V-R = 0.49 ± 0.05 assumed. H_R = 11.64 ± 0.03.


   2423 Ibarruri                      
        Binzel 2019                    MITHNEOS Method: VIS


   2449 Kenos                         
        Binzel 2019                    MITHNEOS Method: eVISNIR


   2453 Wabash                        
        Galad 2010c                    Combined with data from Pray (2006c)


   2462 Nehalennia                    
        Szabo 2016 entries are based on Kepler 2 data. Most objects did not have a reported
        period/amplitude.


   2483 Guinevere                     
        The objects under Sonnett 2015 were observed in the W3 (12 um) band by WISE. The amplitude
        given is the maximum range of values, not the range of a fitted lightcurve. No periods were
        given for the data.


   2500 Alascattalo                   
        Bentz 2023                     Period using V data. R data gave P = 2.786(0.050), A =
                                       0.18(0.02).


   2575 Bulgaria                      
        Athanasopoulos 2022            Paper gave Beta1 = 91, which is not allowed in LCDB, so a
                                       value of 90 was entered.


   2577 Litva                         
        Warner 2009q                   P2 is assumed to be due to the rotation of the secondary.
                                       There is slight evidence that the secondary may be tidally
                                       locked and, therefore, P2 is due to the rotation of a third
                                       body in the system.

        Merline 2013b                  P_Orb(S2): 214 d (107 d). D(S2): 1.2 km.

        Merline 2013c                  P_Orb(S2): 214 d (107 d). D(S2): 1.2 km. D(S1): 1.4 km.

        Binzel 2019                    MITHNEOS Method: VIS


   2608 Seneca                        
        Binzel 2019                    MITHNEOS Method: TAXON


   2629 Rudra                         
        Binzel 2019                    MITHNEOS Method: VIS


   2691 Sersic                        
        Oey 2016a                      No mutual events seen but second period found. See binary
                                       data table.


   2712 Keaton                        
        This note applies to all Chang 2019 (ArXiv:1901.08719) detail records: The Chang et al. U
        codes are not necessarily those given in the LCDB. Initial bulk data entry assigned U = 2
        pending individual review.


   2744 Birgitta                      
        Binzel 2019                    MITHNEOS Method: VIS


   2754 Efimov                        
        Pray 2006g                     Ds/Dp = 0.20 ± 0.03.


   2760 Kacha                         
        Warner 2021b                   Weak secondary period of 15.63 h, 0.04 mag provided better
                                       fit but is likely an artifcat of the Fourier anlayis.


   2802 Weisell                       
        Behrend 2006web                Originally reported as P = 37.74 ± 0.06 h, A = 0.41 ± 0.03
                                       mag. Data forced to fit period found in 2011.


   2815 Soma                          
        Pollock 2011                   Ds/Dp = 0.25 ± 0.02.


   2847 Parvati                       
        Behrend 2018web                Overlooked binary?


   2867 Steins                        
        Jorda 2008                     Lightcurve data obtained by OSIRIS/Rosetta spacecraft. The
                                       phase angle was 41.7 as seen from the craft, not the Earth.

        Lamy 2008a                     Axis ratios: a/b: 1.17; a/c: 1.25. Size: 5.73 ± 0.52, 4.95 ±
                                       0.45, 4.58 ± 0.41 km

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   2881 Meiden                        
        Polakis 2017a                  The assignment of the primary and secondary periods may be
                                       reversed, i.e., the longer of the two periods may be the
                                       primary. The rotation of the satellite responsible for events
                                       is locked to the orbital period.


   2897 Ole Romer                     
        Pravec 2019b                   Paired with (182259) 2001 FZ185.


   2937 Gibbs                         
        Warner 2019r                   Second period found but cause not established. Could be a
                                       tumbler or binary without mutual events.

        Warner 2019r                   The U = 3- rating is for the primary period, which is clearly
                                       established (unless the object is a low-level tumbler).


   2968 Iliya                         
        Binzel 2019                    MITHNEOS Method: sVIS


   3025 Higson                        
        Behrend 2010web                Originally reported 10.8 h. Updated to fit to period found
                                       with 2016 data.


   3040 Kozai                         
        Binzel 2019                    MITHNEOS Method: VIS


   3073 Kursk                         
        Skiff 2019b                    Lightcurve forced to near primary period of known binary and
                                       shows effects of satellite events.


   3102 Krok                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3103 Eger                          
        Durech 2012                    YORP acceleration: (1.4 ± 0.6) x 10^-8 rad d^-2

        Binzel 2019                    MITHNEOS Method: VISNIR


   3122 Florence                      
        Benner 2017                    P_ORB_Inner: ~8h. P_ORB_Outer: ~24h. Satellites are assumed
                                       to be tidally locked to orbital period.

        Binzel 2019                    MITHNEOS Method: VISNIR


   3138 Ciney                         
        Hills 2014a                    Author reported P = 56.1 h with monomodal lightcurve but 0.56
                                       mag amplitude virtually assures a bimodal curve and,
                                       therefore, double period.


   3157 Novikov                       
        Marchini 2019c                 The period in the work was 9.952 h. However, analysis of the
                                       data by the LCDB authors found that 14.930 h was more likely
                                       correct.


   3198 Wallonia                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3199 Nefertiti                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3200 Phaethon                      
        Ansdell 2014                   Color index values are the average of three values derived
                                       over several years. The errors were added in quadrature.

        Radar Team 2017c               Diameter based on high-res (75m/pixel) images.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Tabeshian 2019                 H-G_B: 14.57(2), 0.00(1); H-G_R:13.28(2),-0.10(1); H-G_I:
                                       13.07(2), -0.08(1).


   3250 Martebo                       
        Alvarez 2014b                  Author found H_R = 10.84. A V-R = 0.38 was assumed to give
                                       H_V = 11.22 ± 0.06.


   3255 Tholen                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3260 Vizbor                        
        Diameter and albedo taken from Warner 2012, which revised WISE diameter and albedo with new
        H-G and Harris and Harris (1997).


   3267 Glo                           
        Binzel 2019                    MITHNEOS Method: VIS


   3287 Olmstead                      
        Binzel 2019                    MITHNEOS Method: VIS


   3288 Seleucus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3309 Brorfelde                     
        Warner 2009i                   Ds/Dp: 0.26 ± 0.02


   3343 Nedzel                        
        Binzel 2019                    MITHNEOS Method: VIS


   3352 McAuliffe                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3361 Orpheus                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   3362 Khufu                         
        Binzel 2019                    MITHNEOS Method: VIS


   3401 Vanphilos                     
        Binzel 2019                    MITHNEOS Method: VIS


   3402 Wisdom                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3443 Leetsungdao                   
        Binzel 2019                    MITHNEOS Method: VIS


   3481 Xianglupeak                   
        Pravec 2012web                 A single suspect attentuation was seen.


   3494 Purple Mountain               
        Cantu 2016                     Authors adopted shorter (monomodal) period. However, the
                                       amplitude and phase angle dictated a bimodal solution at the
                                       longer period.


   3548 Eurybates                     
        Noll 2020a                     Obs date is for first detection.


   3551 Verenia                       
        Binzel 2019                    MITHNEOS Method: TAXON


   3552 Don Quixote                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   3553 Mera                          
        Binzel 2019                    MITHNEOS Method: NIR


   3554 Amun                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3581 Alvarez                       
        Binzel 2019                    MITHNEOS Method: VIS


   3623 Chaplin                       
        Marchis 2012                   Hv assumed V-R = 0.54.


   3635 Kreutz                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3669 Vertinskij                    
        Behrend 2020web                Period matches orbital period of satellite (Christmann et al.
                                       2020; CBET 4749).


   3671 Dionysus                      
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


   3673 Levy                          
        Pravec 2007web                 Refinements on the original parameters reported by Pray et al
                                       in CBET 1165.


   3674 Erbisbuhl                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3691 Bede                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3704 Gaoshiqi                      
        Pravec 2010web                 Systematic residuals seen, possibly due to another lightcurve
                                       component, but no good solution could be found.


   3737 Beckman                       
        Binzel 2019                    MITHNEOS Method: VIS


   3749 Balam                         
        Merline 2002a                  Estimated size of satellite: 1.5 km.

        Marchis 2008b                  This is a trinary system, with a more distant satellite
                                       reported via AO observations (2002, IAUC 7827)

        Behrend 2014web                Lightcurve shows mutual events (Amp_max = 0.46 ± 0.03) but
                                       rotation of primary not isolated.

        Pravec 2019b                   Paired with (312497) 2009 BR60.

        Pravec 2019b                   Binary information for this record is for the second
                                       satellite in (3749) Balam system.


   3752 Camillo                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   3753 Cruithne                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3757 Anagolay                      
        Binzel 2019                    MITHNEOS Method: TAXON


   3761 Romanskaya                    
        Clark 2020                     Results table gives P = 9.456 h.


   3782 Celle                         
        Marchis 2012                   Hv found using assumged V-I = 0.88.


   3792 Preston                       
        Pravec 2016web                 The 23.8 h orbital period is based on a bimodal solution
                                       derived from a monomodal solution of 11.91 h. Possible, very
                                       shallow mutual events.

        Benishek 2017c                 If not binary, the two periods may indicate low-level
                                       tumbling.


   3800 Karayusuf                     
        Warner 2008m                   Two possible mutual events. Insufficient data to calculate a
                                       period.

        Binzel 2019                    MITHNEOS Method: VIS


   3833 Calingasta                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   3841 Dicicco                       
        Klinglesmith 2015d             Ds/Dp in Binary table is a minimum.


   3854 George                        
        Warner 2006f                   Suspicious attenutations but insufficient data for valid
                                       analysis.


   3858 Dorchester                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   3908 Nyx                           
        Binzel 2019                    MITHNEOS Method: VISNIR


   3912 Troja                         
        Benishek 2021h                 Lightcurves availalbe at
                                       http://www.asu.cas.cz/~asteroid/03912_2021a_p1.png
                                       http://www.asu.cas.cz/~asteroid/03912_2021a_porb.png


   3920 Aubignan                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3951 Zichichi                      
        Franco 2018c                   Some attenuations due to satellite observed. Period is based
                                       on single-period solution.


   3982 Kastel'                       
        Pravec 2005b                   Second period in binary table may be 2.918 h.


   3988 Huma                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4015 Wilson-Harrington             
        Also know as 107P/Wilson-Harrington. It has been observed to exhibit a cometary appearance.
        Photometry of this object may be contaminated by unresolved coma and not represent net
        nucleus brightness.

        Urakawa 2011                   The authors reported pole solutions. However, these are not
                                       considered reliable since they are based on data that are too
                                       limited for proper spin axis modeling.

        Urakawa 2012                   The authors provided four possible solutions that involved
                                       either tumbling, a binary object, or a single body in PA
                                       rotation. The spin axis and period are for for the PA
                                       solution.

        Binzel 2019                    MITHNEOS Method: eVISNIR 'Worked as' field is '1979 VA=165P'
                                       in original paper.


   4022 Nonna                         
        Behrend 2013web                Authors reported P = 1.31 h; this seems unlikely and so the
                                       double period was entered for the details record.


   4034 Vishnu                        
        Binzel 2019                    MITHNEOS Method: NIR


   4055 Magellan                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4142 Dersu-Uzala                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   4162 SAF                           
        Dose 2022b                     Author gave 3.850 h for a monomodal lightcurve. There are
                                       indications that a doubled-period, with bimodal lightcurve,
                                       might be preferred.


   4179 Toutatis                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4183 Cuno                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4197 Morpheus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4205 David Hughes                  
        Binzel 2019                    MITHNEOS Method: VIS


   4225 Hobart                        
        Behrend 2023web                Reported as P = 8.3202 h. This gives either a 3 or 6 maximum
                                       lightcurve (depending on the impretation of the maximums).
                                       The period given is 2/3 the reported period with a bimodal
                                       lightcurve.


   4263 Abashiri                      
        Pravec 2012web                 A few deviations were see but nothing significant or
                                       convincing.


   4276 Clifford                      
        Binzel 2019                    MITHNEOS Method: VIS


   4336 Jasniewicz                    
        Owings 2018                    The longer period is determined from data and based on
                                       removing one night from the lightcurve.


   4337 Arecibo                       
        Gault 2022                     Second, confirming occulation on 2021 June 9. Dp = 24.4
                                       Ãƒâ€šÃ‚Â± 0.6 km, Ds = 13.0 Ãƒâ€šÃ‚Â± 1.5 (assuming circular
                                       shapes derived from occltation chords.


   4341 Poseidon                      
        Binzel 2019                    MITHNEOS Method: VIS


   4370 Dickens                       
        Benishek 2021j                 Secondary outside of events shows 0.04 mag lightcurve, a/b =
                                       1.3 Ã‚Â± 0.1.

        Pravec 2021web                 Tenative lightcurves at
                                       http://www.asu.cas.cz/~asteroid/04370_2021a_p1.png
                                       http://www.asu.cas.cz/~asteroid/04370_2021a_porb.png


   4401 Aditi                         
        Binzel 2019                    MITHNEOS Method: NIR


   4435 Holt                          
        Stephens 2018c                 Mutual events not tied to orbital period seen: possible
                                       second satellite.

        Stephens 2018g                 Attenuations not tied to the orbital period may indicate a
                                       second satellite. See original paper for the evolution of the
                                       primary lightcurve and mutual events.

        Binzel 2019                    MITHNEOS Method: VIS


   4450 Pan                           
        Carbognani 2008b               Values for G and Pv were assumed based on Wisniewski (1997).

        Binzel 2019                    MITHNEOS Method: NIR


   4451 Grieve                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   4486 Mithra                        
        The amplitude, A = 0.5, is an estimate based on the derived shape of the asteroid and an
        equatorial view.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4492 Debussy                       
        Marchis 2012                   Hv found using V-R 0.54.


   4495 Dassanowsky                   
        Ambiguity is for P1. Binary status not in doubt.

        Warner 2019i                   Ambiguity is for P1. Adopted period is favored because of
                                       estimated size ratio of system and binary modeling (Pravec et
                                       al., 2010)


   4503 Cleobulus                     
        Binzel 2019                    MITHNEOS Method: VIS


   4524 Barklajdetolli                
        Athanasopoulos 2022            The original paper reported Beta2 = 93 deg. Values |beta| >
                                       90 are not allowed in the LCDB and so B2 = 90 was used.


   4528 Berg                          
        Fornas 2023a                   Polakis data (ALCDEF, 2018 Feb) included in solution.


   4541 Mizuno                        
        Pray 2015b                     Ds/Dp >= 0.24


   4544 Xanthus                       
        Binzel 2019                    MITHNEOS Method: NIR


   4555 Josefaperez                   
        Pravec 2007web                 Variations in mean levels of the calibrated Ondrejov R data
                                       suggest that there may be a rotation of an unresolved
                                       satellite.


   4558 Janesick                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4587 Rees                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4660 Nereus                        
        The pV = 0.3 is based on Pravec et al. (2021web) assumption of G = 0.43. Using the default
        pV = 0.2 gives a diameter of 0.516 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4666 Dietz                         
        Pravec 2015web                 One suspected event captured.

        Oey 2018a                      Data from 2011 and 2015 included in analysis. Possible third
                                       period seen in 2015 and 2018 data.

        Warner 2021g                   Alternate orbital solution is 33.4 h, which is near that
                                       found in 2018 and for which the mutual events were much
                                       better defined.


   4688 1980 WF                       
        This note applies to all Binzel 2019 (2019Icar..324...41B) detail records:  VIS indicates
        visible data only.  NIR indicates near-infrared data only.  VISNIR indicates both. eVISNIR
        indicates the visible portion of the spectrum is from the Eight-Color Asteroid Survey (ECAS,
        Zellner et al. 1985) sVis indicates the visible portion of the spectrum is from the Sloan
        Digital Sky Survey (SDSS, Ivezic et al. 2001). TAXON indicates the type is reported in the
        literature; see the source listed in the 'Taxon' reference column of the original file.  For
        visible data only (VIS), the taxonomic type is from the Bus classification system (Bus and
        Binzel 2002). For visible plus near-infrared data (VISNIR), the taxonomic type is from the
        Bus-DeMeo classification system (DeMeo et al. 2009).  '-comp' refers to the broad taxonomic
        complex. When multiple taxonomic classes are listed, they are in subjective order of most
        likely type first. ':' indicates the assignment is uncertain.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4690 Strasbourg                    
        Warner 2011j                   Multiple solutions possible because of the limited data set.
                                       Analysis by Petr Pravec.


   4708 Polydoros                     
        Stephens 2018i                 Period taken from plot. Results table and text each have a
                                       different period.


   4718 Araki                         
        Pravec 2017web                 The nature of the two periods is uncertain. They could be the
                                       result of a binary or low level tumbling, thus this record
                                       carries both flags.


   4729 Mikhailmil'                   
        Ruthroff 2012a                 Lightcurve has very unusual shape. The period could really
                                       lie between 15-30 h.


   4765 Wasserburg                    
        Pravec 2019b                   Paired with (350716) 2001 XO105.


   4775 Hansen                        
        Binzel 2019                    MITHNEOS Method: sVISNIR


   4788 Simpson                       
        Sogorb 2021                    Third period (3.1506 h) may be due to eclipsing/occultating
                                       secondary or a third body.


   4905 Hiromi                        
        Pravec 2019b                   Paired with (7813) Anderserikson.


   4910 Kawasato                      
        Binzel 2019                    MITHNEOS Method: VIS


   4947 Ninkasi                       
        Binzel 2019                    MITHNEOS Method: VIS


   4953 1990 MU                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   4954 Eric                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4957 Brucemurray                   
        Binzel 2019                    MITHNEOS Method: VIS


   4995 Griffin                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5003 Silvanominuto                 
        Waszczak (2016) H values are based on G12 system. The G12 value is given instead of G and
        carries 'G' for the source flag. The G2 value is NULL. The LCDB U value is based on the
        Waszczak et al. 'relflag' value, with relflag = 0 given U = 1 and relflag = 1 given U = 2


   5011 Ptah                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   5026 Martes                        
        Pravec 2019b                   Paired with 2005 WW113.


   5066 Garradd                       
        Binzel 2019                    MITHNEOS Method: sVIS


   5076 Lebedev-Kumach                
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5104 Skripnichenko                 
        Behrend 2023web                Reported as 5.56457 h. The amplitude and high degree of
                                       symmentry of the quadramodal lightcurve make this unlikely.


   5131 1990 BG                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5143 Heracles                      
        Taylor 2012b                   Dp = 3.6 ± 1.2 km; Ds = 0.6 ± 0.3 km. Orbital period of 16 h
                                       is based on period 14-17 h. A period of 40-57 h cannot be
                                       excluded, but it is inconsistent with the assumption of a
                                       synchronously rotating secondary.

        Binzel 2019                    MITHNEOS Method: VISNIR


   5145 Pholus                        
        Tegler 2005                    Dimensions (diameters) determined by calculation to be 310 X
                                       160 x 150 km. This gives an effective spheroidal diameter of
                                       ~190 km.

        Belskaya 2010b                 To derive H, used V-R=0.77 and phase coefficient (not G) of
                                       0.083 mag/degree.


   5230 Asahina                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5247 Krylov                        
        Lee 2020                       P = 82.28 is the strongest apparent period, the conjunction
                                       of the period of rotation (368.7 h) and rotation (67.27 h).


   5261 Eureka                        
        Binzel 2019                    MITHNEOS Method: VISNIR

        Skiff 2019b                    Raw plot shows total eclipse/occultation due to satellite.

        Skiff 2019b                    Raw plot shows mutual event due to satellite.


   5275 Zdislava                      
        Binzel 2019                    MITHNEOS Method: VIS


   5332 Davidaguilar                  
        Binzel 2019                    MITHNEOS Method: NIR


   5349 Paulharris                    
        Binzel 2019                    MITHNEOS Method: VIS


   5381 Sekhmet                       
        Binzel 2019                    MITHNEOS Method: NIR


   5384 Changjiangcun                 
        The low WISE and AKARI albedos indicate that C-type is a better choice rather than the LCDB
        default of ES for Hungaria members.


   5392 Parker                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   5402 Kejosmith                     
        Benishek 2018j                 The ambiguity is for Porb. It may be 32.62 h instead of the
                                       adopted 16.31 h.


   5407 1992 AX                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5425 Vojtech                       
        Vander Haagen 2012a            Author reported a trimodal solution of 3.972 h. This is
                                       considered highly unlikely.


   5496 1973 NA                       
        Binzel 2019                    MITHNEOS Method: NIR


   5510 1988 RF7                      
        Binzel 2019                    MITHNEOS Method: VIS


   5535 Annefrank                     
        Hillier 2011                   Stardust and ground-based observations.


   5573 Hilarydownes                  
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5585 Parks                         
        Binzel 2019                    MITHNEOS Method: VIS


   5587 1990 SB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5604 1992 FE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5620 Jasonwheeler                  
        Binzel 2019                    MITHNEOS Method: NIR


   5626 Melissabrucker                
        Binzel 2019                    MITHNEOS Method: VISNIR


   5642 Bobbywilliams                 
        Binzel 2019                    MITHNEOS Method: NIR


   5645 1990 SP                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5646 1990 TR                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5649 Donnashirley                  
        Binzel 2019                    MITHNEOS Method: VIS


   5653 Camarillo                     
        Binzel 2019                    MITHNEOS Method: NIR


   5656 Oldfield                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5660 1974 MA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5674 Wolff                         
        Aznar 2016b                    Ds/Dp >= 0.80


   5693 1993 EA                       
        Binzel 2019                    MITHNEOS Method: eVISNIR


   5720 Halweaver                     
        Binzel 2019                    MITHNEOS Method: NIR


   5732 1988 WC                       
        Binzel 2019                    MITHNEOS Method: VIS


   5751 Zao                           
        Binzel 2019                    MITHNEOS Method: VIS


   5786 Talos                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   5797 Bivoj                         
        Binzel 2019                    MITHNEOS Method: TAXON


   5817 Robertfrazer                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   5828 1991 AM                       
        Binzel 2019                    MITHNEOS Method: VIS


   5836 1993 MF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5867 1988 RE                       
        Binzel 2019                    MITHNEOS Method: NIR


   5870 Baltimore                     
        Binzel 2019                    MITHNEOS Method: VIS


   5899 Jedicke                       
        Warner 2010h                   The amplitude of the primary was too low to establish a
                                       period with certainty. The mutual events, however, were
                                       well-defined.

        Warner 2010n                   The amplitude of the primary was too low to establish a
                                       period with certainty. The mutual events, however, were
                                       well-defined.


   5968 Trauger                       
        Warner 2014d                   Unexplained 'event' on Sep 5. Possible period solutions
                                       assuming a satellite are P_orb = 15.9 or 31.7 h.


   6037 1988 EG                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6041 Juterkilian                   
        Binzel 2019                    MITHNEOS Method: sVIS


   6042 Cheshirecat                   
        Binzel 2019                    MITHNEOS Method: sVIS


   6047 1991 TB1                      
        Binzel 2019                    MITHNEOS Method: VIS


   6053 1993 BW3                      
        Warner 2015s                   Result of combining data sets from 2015 January and March.

        Binzel 2019                    MITHNEOS Method: TAXON


   6063 Jason                         
        Warner 2017n                   Radar could not confirm long period.

        Binzel 2019                    MITHNEOS Method: NIR


   6070 Rheinland                     
        Vokrouhlicky 2011              H_R actually found. Authors used V-R = 0.49 ± 0.05 to convert
                                       to H.

        Vokrouhlicky 2017b             See paper for discussion of pole solution uncertainties.

        Pravec 2019b                   Paired with (54827) Kurpfalz.


   6084 Bascom                        
        Pravec 2012a                   Residual variations of 0.02 mag may indicate rotation of a
                                       satellite.


   6170 Levasseur                     
        Binzel 2019                    MITHNEOS Method: sVIS


   6178 1986 DA                       
        Binzel 2019                    MITHNEOS Method: NIR


   6183 Viscome                       
        Binzel 2019                    MITHNEOS Method: sVIS


   6186 Zenon                         
        Benishek 2017b                 S1 has amplitude of 0.04 mag.


   6239 Minos                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   6261 Chione                        
        Binzel 2019                    MITHNEOS Method: sVIS


   6369 1983 UC                       
        Pravec 2019b                   Paired with (510132) 2010 UY57. The Observing Circumstances
                                       are for lightcurves from 2013.


   6386 Keithnoll                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   6411 Tamaga                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   6444 Ryuzin                        
        Binzel 2019                    MITHNEOS Method: sVIS


   6455 1992 HE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6456 Golombek                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a p_V = 0.18.

        Binzel 2019                    MITHNEOS Method: VISNIR


   6489 Golevka                       
        Binzel 2019                    MITHNEOS Method: TAXON


   6500 Kodaira                       
        Binzel 2019                    MITHNEOS Method: VIS


   6523 Clube                         
        Binzel 2019                    MITHNEOS Method: sVIS


   6569 Ondaatje                      
        Binzel 2019                    MITHNEOS Method: VIS


   6585 O'Keefe                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6611 1993 VW                       
        Pravec 2005web                 The second period maybe the secondary's rotation or the
                                       orbtial period.

        Binzel 2019                    MITHNEOS Method: VISNIR


   6764 Kirillavrov                   
        Polakis 2022a                  Analysis of TESS data (Pal et al, 2020, Ap. J. 247, A26).


   6809 Sakuma                        
        Pravec 2018web                 Suspected mutual events observed on two nights.


   6847 Kunz-Hallstein                
        Binzel 2019                    MITHNEOS Method: VIS


   6909 Levison                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7002 Bronshten                     
        Binzel 2019                    MITHNEOS Method: VIS


   7025 1993 QA                       
        Binzel 2019                    MITHNEOS Method: sVIS


   7079 Baghdad                       
        Binzel 2019                    MITHNEOS Method: sVIS


   7088 Ishtar                        
        Binzel 2019                    MITHNEOS Method: VIS


   7092 Cadmus                        
        Binzel 2019                    MITHNEOS Method: NIR


   7132 Casulli                       
        Franco 2020e                   The original gives Ds/Dp ~ 0.21. The 0.11 mag attenuation
                                       gives Ds/Dp ~ 0.33. The latter is used in the lc_binaries
                                       table.


   7165 Pendleton                     
        Behrend 2023web                Data show possible binary events.


   7187 Isobe                         
        Warner 2011o                   Weak secondary period: P = 16.33 ± 0.04 h, A = 0.12 ± 0.01
                                       mag.

        Warner 2011o                   Weak secondary period: P = 16.378 ± 0.05 h, A = 0.05 ± 0.01
                                       mag.


   7304 Namiki                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   7307 Takei                         
        Benishek 2021e                 Secondary has lightcurve amplitude (in the combined primary
                                       plus secondary lightcurve) of 0.05 mag.


   7335 1989 JA                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   7336 Saunders                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   7341 1991 VK                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7343 Ockeghem                      
        Pravec 2019b                   Paired with (154634) 2003 XX38.


   7350 1993 VA                       
        Binzel 2019                    MITHNEOS Method: NIR


   7358 Oze                           
        Binzel 2019                    MITHNEOS Method: VISNIR


   7393 Luginbuhl                     
        Warner 2019k                   Out of event satellite lightcurve indicates elongation of
                                       about 1.7:1


   7474 1992 TC                       
        Binzel 2019                    MITHNEOS Method: VIS


   7480 Norwan                        
        Binzel 2019                    MITHNEOS Method: VIS


   7482 1994 PC1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   7488 Robertpaul                    
        Stephens 2022e                 P2 isn't a formal solution, just that one that, when
                                       subtracted, results in a U = 3- P1.


   7517 Alisondoane                   
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   7560 Spudis                        
        Warner 2013d                   There is a weak secondary period of 22.6 h. The 2004
                                       apparition showed a possible binary with orbital period of
                                       23.4 h.


   7604 Kridsadaporn                  
        Binzel 2019                    MITHNEOS Method: VIS


   7722 Firneis                       
        This applies to all Colazo 2021d entries. There are up to three details entries per object:
        1) H-G using Gaia GR magnitudes, 2) H-G with GR magnitudes transformed to V and adding
        ground-based data to include phase angles < 10 deg, and 3) H-G1,G2 using the same magnitudes
        as in 2. Only results where there were valid numbers for H and HErr and the G or G1/G2
        errors were <= 1.0 were included in the LCDB entries. H/HErr were rounded to two decimal
        places and G/GErr values were rounded to three decimal places. For a new summary record, the
        MPCOrb values are used for H and G for groups 1 and 3. This provides the necessary
        consitency for H when generating frequency-diameter plots from LCDB data, which have have
        been historically based on the H(V)-G system. For the Details record, the H Band is 'GR' for
        group 1 and 'V' for groups 2 and 3. To help convey that the V magnitudes were derived from
        GR and assumed V-R magnitudes, the H Method is 'D' (Derived). The G Method will be empty for
        groups 1 and 2 since, regardless


   7753 1988 XB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7757 Kameya                        
        Warner 2011web                 Data too noisy to give reasonable period or amplitude.


   7758 Poulanderson                  
        Warner 2012m                   Only one event well seen, maybe a second. Several other
                                       orbital period solutions fit, ranging out to about 100 hours.
                                       


   7760 1990 RW3                      
        Galad 2010c                    Combined with data from Pray (2006f)


   7813 Anderserikson                 
        Pravec 2019b                   Paired with (4905) Hiromi.


   7818 Muirhead                      
        Binzel 2019                    MITHNEOS Method: sVIS


   7822 1991 CS                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7888 1993 UC                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7889 1994 LX                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7977 1977 QQ5                      
        Binzel 2019                    MITHNEOS Method: TAXON


   8013 Gordonmoore                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   8014 1990 MF                       
        Binzel 2019                    MITHNEOS Method: NIR


   8034 Akka                          
        Binzel 2019                    MITHNEOS Method: TAXON


   8037 1993 HO1                      
        Binzel 2019                    MITHNEOS Method: VIS


   8167 Ishii                         
        Pravec 2021web                 Two attenutions suspected on Feb 6 and 9.


   8176 1991 WA                       
        Binzel 2019                    MITHNEOS Method: TAXON


   8201 1994 AH2                      
        Binzel 2019                    MITHNEOS Method: TAXON


   8306 Shoko                         
        Polishook 2014a                Likely mutual events seen twice, but insufficient data to
                                       determine the orbital period for a satellite.

        Pravec 2014a                   Possible third body.

        Pravec 2019b                   Paired with 2011 SR158.


   8345 Ulmerspatz                    
        The lightcurves from the 2011-2012 apparition give strong indications that this asteroid
        might be a tidally-locked binary of nearly equal sized components, similar to 90 Antiope.

        Klinglesmith 2012c             When using the full data set, P = 17.1192 ± 0.0008 h.


   8355 Masuo                         
        Binzel 2019                    MITHNEOS Method: sVIS


   8356 Wadhwa                        
        Pravec 2008web                 http://www.asu.cas.cz:80/~asteroid/08356.png


   8369 Miyata                        
        Warner 2011s                   Subtracting a weak secondary period of 49.24 h improves the
                                       RMS fit of the 2.73 h period noticeably.


   8373 Stephengould                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   8444 Popovich                      
        Binzel 2019                    MITHNEOS Method: sVIS


   8566 1996 EN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   8567 1996 HW1                      
        Magri 2011                     Authors give ellipsoid of 3.8x1.6x1.5 km, which gives an
                                       effective spheroidal diameter of about 2 km.  Composite
                                       lightcurves were not provided, only overlays of the
                                       lightcurve data over the model curve. The U=3 rating refers
                                       to the overall quality of the data set used to find the pole,
                                       shape, and sidereal period.

        Trilling 2016                  This applies to all Trilling 2016 (AJ 152): the listed errors
                                       for the diameter and albedo are the larger of the ± values,
                                       which were not the same.

        Binzel 2019                    MITHNEOS Method: VISNIR


   8651 Alineraynal                   
        Binzel 2019                    MITHNEOS Method: VIS


   8828 1988 RC7                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   8861 Jenskandler                   
        Hayes-Gehrke 2023c             P = 4.500 is a trimodal solution.


   8864 1991 VU                       
        The albedo error given for Masiero 2017 is the maximum possible value when converting from
        albedo values from log space to value space.


   9068 1993 OD                       
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2019b                   Paired with (455327) 2002 OP28.

        Pravec 2019b                   Paired with (455327) 2002 OP28.


   9069 Hovland                       
        Marchis 2012                   Hv assumed V-R = 0.54.


   9082 Leonardmartin                 
        Binzel 2019                    MITHNEOS Method: VIS


   9162 Kwiila                        
        Binzel 2019                    MITHNEOS Method: TAXON


   9202 1993 PB                       
        Binzel 2019                    MITHNEOS Method: sVIS


   9400 1994 TW1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   9671 Hemera                        
        Binzel 2019                    MITHNEOS Method: sVIS


   9783 Tensho-kan                    
        Pravec 2019b                   Paired with (348018) 2003 SF334.


   9856 1991 EE                       
        Binzel 2019                    MITHNEOS Method: TAXON


   9881 Sampson                       
        Binzel 2019                    MITHNEOS Method: sVIS


   9950 ESA                           
        Binzel 2019                    MITHNEOS Method: NIR


   9969 Braille                       
        Binzel 2019                    MITHNEOS Method: VIS


   9992 1997 TG19                     
        Higgins 2006f                  Incorrectly referenced in text as 1997 TH19.

        Binzel 2019                    MITHNEOS Method: NIR


  10051 Albee                         
        Binzel 2019                    MITHNEOS Method: sVIS


  10115 1992 SK                       
        Binzel 2019                    MITHNEOS Method: sVISNIR

        Durech 2022                    YORP Parameter: 8.3(6) * (10^8 rad d^-2)


  10123 Fideoja                       
        Pravec 2019b                   Paired with (117306) 2004 VF21.


  10132 Lummelunda                    
        Benishek 2018f                 See original paper for evolution of the primary lightcurve
                                       and attenuation events.

        Salvaggio 2018b                Shorter period in ambiguous table comes from lightcurve plot
                                       while longer period in detail record comes from text.


  10145 1994 CK1                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  10150 1994 PN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  10165 1995 BL2                      
        Binzel 2019                    MITHNEOS Method: VIS


  10199 Chariklo                      
        Belskaya 2010b                 To derive H, used V-R=0.48 and phase coefficient (not G) of
                                       0.06 mag/degree.


  10247 Amphiaraos                    
        McNeill 2021                   This note applies to all entries for McNeill et al. (2021;
                                       Plan. Sci. J. 2, A6). The H-G (Bowell) model was used for
                                       finidng Hc/Ho and, from all appearances, Go not Gv. Table 1
                                       lists Hv values taken from the JPL database and not Ho (the
                                       orange data being far more prevalent) or Hc. The error for Hv
                                       was presumed to be 0.05 mag


  10261 Nikdollezhal'                 
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  10295 Hippolyta                     
        Binzel 2019                    MITHNEOS Method: NIR


  10296 Rominadisisto                 
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  10302 1989 ML                       
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2022i                   Final solution when using additive period anlaysis required
                                       P3 = 18.90, A3=0.15.


  10502 Armaghobs                     
        Binzel 2019                    MITHNEOS Method: sVIS


  10563 Izhdubar                      
        Binzel 2019                    MITHNEOS Method: TAXON


  10779 1991 LW                       
        Warner 2011o                   One-night stand. Period is based on a half-period analysis.


  11001 Andrewulff                    
        Pravec 2012web                 Partial attenuations seen but not enough to confirm binary
                                       status.


  11054 1991 FA                       
        Binzel 2019                    MITHNEOS Method: NIR


  11066 Sigurd                        
        Binzel 2019                    MITHNEOS Method: VISNIR


  11284 Belenus                       
        Binzel 2019                    MITHNEOS Method: NIR


  11286 1990 RO8                      
        Pravec 2019b                   Paired with (59394) 1999 FZ23.


  11311 Peleus                        
        Binzel 2019                    MITHNEOS Method: VIS


  11351 Leucus                        
        Mottola 2020                   V-SR: 0.313 Ãƒâ€šÃ‚Â± 0.021


  11398 1998 YP11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  11405 1999 CV3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  11500 Tomaiyowit                    
        Binzel 2019                    MITHNEOS Method: VIS


  11677 1998 DY4                      
        Pravec 2019b                   Paired with (412065) 2013 ET86.

        Pravec 2019b                   Paired with (412065) 2013 ET86.


  11836 Eileen                        
        Binzel 2019                    MITHNEOS Method: sVIS


  11842 Kap'bos                       
        Ye 2011                        Asteroid pair with (228747) 2002 VH3, for which Ye found B-V
                                       = 0.704 ± 0.154, V-R = 0.480 ± 0.057, and V-I = 0.829 ±
                                       0.111.


  11885 Summanus                      
        Binzel 2019                    MITHNEOS Method: NIR


  12016 Green                         
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  12326 Shirasaki                     
        Pray 2017a                     Secondary period may be due to rotation of the satellite or a
                                       third body. If the former, the system would be
                                       fully-asynchronous and not singly-asychronous.


  12376 Cochabamba                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  12538 1998 OH                       
        Vaduvescu 2017                 Sloan g magnitudes

        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2019h                   Two close solutions that are not harmonically related. See
                                       the binaries file. The two periods could also be the result
                                       of tumbling. Both possibilties fit the data.

        Warner 2019p                   The split-halves plot for 5.16 h essentially duplicates the
                                       two halves. In this case, the shorter period was adopted.


  12711 Tukmit                        
        Binzel 2019                    MITHNEOS Method: VISNIR


  12923 Zephyr                        
        Binzel 2019                    MITHNEOS Method: NIR


  13123 Tyson                         
        Pravec 2022web                 No lightcurve for suspected secondary period.


  13186 1996 UM                       
        Wang 2021                      Sideral period for (38, +35): 4.29828 h


  13284 1998 QB52                     
        Pravec 2019b                   Paired with (154828) 2004 RT8.

        Pravec 2019b                   Paired with (154828) 2004 RT8.


  13331 1998 SU52                     
        Warner 2011k                   A weak secondary period of ~15.1 h was observed but could not
                                       be explained.


  13355 1998 TP17                     
        Pravec 2023web                 Second period is well-established. It could be due to
                                       tumbling or a satellite, therefore, the asteroid is listed as
                                       both types.


  13553 Masaakikoyama                 
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2019b                   Single period found 39 h, very similar to Pravec et al. 2005.


  13651 1997 BR                       
        Binzel 2019                    MITHNEOS Method: TAXON


  13732 Woodall                       
        Ye 2011                        Asteroid pair with (1979) Sakharov, for which Ye found B-V =
                                       1.086 and V-R = 0.409.


  13819 1999 SX5                      
        Binzel 2019                    MITHNEOS Method: sVIS


  14017 1994 NS                       
        Binzel 2019                    MITHNEOS Method: sVIS


  14222 1999 WS1                      
        Binzel 2019                    MITHNEOS Method: NIR


  14309 Defoy                         
        Binzel 2019                    MITHNEOS Method: sVIS


  14395 Tommorgan                     
        Warner 2013d                   Second period of 40.4 provided by P. Pravec. The second
                                       solution is not unique. Others are possible.


  14402 1991 DB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  14581 1998 RT4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  14806 1981 EV25                     
        Pravec 2019b                   Paired with (496028) 2008 SC9.


  14827 Hypnos                        
        Binzel 2019                    MITHNEOS Method: TAXON


  14868 1990 RA7                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  14875 1990 WZ1                      
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


  14923 1994 TU3                      
        Warner 2009b                   Recalibration of comp star mags led to different period.


  14982 1997 TH19                     
        Binzel 2019                    MITHNEOS Method: sVIS


  15107 Toepperwein                   
        Pravec 2019b                   Paired with (291188) 2006 AL54.

        Pravec 2021b                   Asteroid pair with (291188) 2006 AL54.


  15350 Naganuma                      
        Pravec 2010web                 Period taken from 2005 observations.


  15430 1998 UR31                     
        Pravec 2010web                 Brightness drops by >0.10 mag seen on 2010-05-06 and 07, but
                                       period not established.


  15607 2000 GA124                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  15609 Kosmaczewski                  
        Binzel 2019                    MITHNEOS Method: sVIS


  15700 1987 QD                       
        Durkee 2010c                   Two possible periods for the orbit were 50.3 and 62.9 h.
                                       Neither could be conclusively established.

        Binzel 2019                    MITHNEOS Method: sVIS


  15745 Yuliya                        
        Warner 2018m                   The primary and orbital period were found by forcing the data
                                       to fit near the periods found by Aznar et al. (2018). The
                                       listed primary period is one of dozens of possible solutions.
                                       

        Binzel 2019                    MITHNEOS Method: VISNIR


  15778 1993 NH                       
        Warner 2015e                   Possible wide binary. The long period is the rotation of the
                                       primary.


  15817 Lucianotesi                   
        Binzel 2019                    MITHNEOS Method: VIS


  15822 Genefahnestock                
        Warner 2011c                   Suspected events seen on three nights in 2010 mid-June. None
                                       seen in 2010 late June or early July.


  16064 Davidharvey                   
        Binzel 2019                    MITHNEOS Method: VIS


  16126 1999 XQ86                     
        Pravec 2019b                   Paired with 2015 AH1.


  16142 Leung                         
        Binzel 2019                    MITHNEOS Method: sVIS


  16426 1988 EC                       
        Diameter and albedo based on H from Warner (2012) and application of Harris and Harris
        (1997) correction to WISE diameter and albedo.


  16635 1993 QO                       
        Binzel 2019                    MITHNEOS Method: sVIS


  16636 1993 QP                       
        Binzel 2019                    MITHNEOS Method: NIR


  16657 1993 UB                       
        Binzel 2019                    MITHNEOS Method: VIS


  16815 1997 UA9                      
        Pravec 2019b                   Paired with (436551) 2011 GD83.


  16816 1997 UF9                      
        Binzel 2019                    MITHNEOS Method: sVIS


  16834 1997 WU22                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  16868 1998 AK8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  16960 1998 QS52                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  17188 1999 WC2                      
        Binzel 2019                    MITHNEOS Method: NIR


  17198 Gorjup                        
        Pravec 2019b                   Paired with (229056) 2004 FC126.


  17274 2000 LC16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  17288 2000 NZ10                     
        Pravec 2019b                   Paired with (203489) 2002 AL80.


  17435 di Giovanni                   
        Binzel 2019                    MITHNEOS Method: sVIS


  17511 1992 QN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  17700 Oleksiygolubov                
        Pray 2018a                     Additional attenuations of 0.14-0.18 mag are not tied to
                                       orbital period and may indicate a third body.


  18106 Blume                         
        Binzel 2019                    MITHNEOS Method: NIR


  18109 2000 NG11                     
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  18172 2000 QL7                      
        Binzel 2019                    MITHNEOS Method: NIR


  18181 2000 QD34                     
        Binzel 2019                    MITHNEOS Method: sVIS


  18514 1996 TE11                     
        Binzel 2019                    MITHNEOS Method: VIS


  18620 1998 DS10                     
        Binzel 2019                    MITHNEOS Method: NIR


  18736 1998 NU                       
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2019m                   Despite the low amplitude of the secondary period, the period
                                       spectrum clearly favors 11.95 h or 23.9 h. The low amplitude
                                       and nearly Earth day period of the secondary lightcurve make
                                       a weak case for being binary.


  18882 1999 YN4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  18916 2000 OG44                     
        Binzel 2019                    MITHNEOS Method: NIR


  19127 Olegefremov                   
        Binzel 2019                    MITHNEOS Method: VISNIR


  19204 Joshuatree                    
        Stephens 2016h                 Main period forced to solution from 2016 data.


  19261 1995 MB                       
        Behrend 2021web                Period was reported by Behrend as 9.130 h. However, that
                                       solution is based on only two nights and at significant phase
                                       angle, ~19 deg, while the 2010 curves from Cabognani and
                                       Owings are at a considerably lower phase angle, 5-6 deg. The
                                       latter, along with fairly large amplitude, would make a
                                       double period, quad extrema, curve very unlikely, bordering
                                       on impossible. On the other hand, the Behrend curve could be
                                       essentially monomodal, with just a very muted secondary
                                       maximum. Also troubling is the very sharp maxima of the
                                       Behrend fit. Sharp minima are expected and can be even more
                                       extreme due to shadowing, but very narrow maxima (broadside
                                       view) are much less expected.


  19289 1996 HY12                     
        Pravec 2019b                   Paired with (278067) 2006 YY40.


  19309 1996 UK1                      
        Galad 2008c                    Several bimodal solutions possible in the range of 4.16-5.91
                                       h.


  19356 1997 GH3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  19388 1998 DQ3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  19764 2000 NF5                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021a                   P3/A3 11.931 h/0.08 mag produces much cleaner P1/P2
                                       lightcurves. It doesn't have a physical nature but filters
                                       the effects of near-Earth day commensurate observations.


  20062 1993 QB3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  20086 1994 LW                       
        Binzel 2019                    MITHNEOS Method: NIR


  20236 1998 BZ7                      
        Binzel 2019                    MITHNEOS Method: TAXON


  20255 1998 FX2                      
        Binzel 2019                    MITHNEOS Method: TAXON


  20384 1998 KW51                     
        Clark 2021                     4 uneven maximums for given period.


  20425 1998 VD35                     
        Binzel 2019                    MITHNEOS Method: VIS


  20429 1998 YN1                      
        Binzel 2019                    MITHNEOS Method: NIR


  20446 1999 JB80                     
        Binzel 2019                    MITHNEOS Method: sVIS


  20452 1999 KG4                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  20691 1999 VY72                     
        Binzel 2019                    MITHNEOS Method: sVIS


  20749 2000 AD199                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  20790 2000 SE45                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  20826 2000 UV13                     
        Binzel 2019                    MITHNEOS Method: VIS


  20882 Paulsanchez                   
        Warner 2019n                   Data split into two sets to show evolution of the mutual
                                       events.


  20958 A900 MA                       
        Binzel 2019                    MITHNEOS Method: sVIS


  21028 1989 TO                       
        Pravec 2019b                   Paired with (481085) 2005 SA135.


  21088 Chelyabinsk                   
        Binzel 2019                    MITHNEOS Method: VISNIR


  21149 Kenmitchell                   
        Warner 2024                    2015 Results: A third period, P3 = 60.4 ± 0.1 h, A3 = 0.16 ±
                                       0.02 mag, was required to get P1/P2 similar to 2023.


  21436 Chaoyichi                     
        Pravec 2019b                   Paired with (334916) 2003 YK39.


  21601 1998 XO89                     
        French 2013                    Authors confirmed that the period in paper's table and not
                                       the one in the lightcurve plot is the correct value.


  21709 Sethmurray                    
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)


  21966 Hamadori                      
        Binzel 2019                    MITHNEOS Method: sVIS


  22099 2000 EX106                    
        Binzel 2019                    MITHNEOS Method: VIS


  22449 Ottijeff                      
        Binzel 2019                    MITHNEOS Method: VIS


  22753 1998 WT                       
        Binzel 2019                    MITHNEOS Method: eVISNIR


  22771 1999 CU3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  22807 1999 RK7                      
        Binzel 2019                    MITHNEOS Method: sVIS


  22891 1999 SO11                     
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


  23183 2000 OY21                     
        Binzel 2019                    MITHNEOS Method: NIR


  23186 2000 PO8                      
        Warner 2021i                   Model dimensions (c = 1): a/b = 1.2, a/c = 2.3.


  23187 2000 PN9                      
        Binzel 2019                    MITHNEOS Method: NIR


  23548 1994 EF2                      
        Binzel 2019                    MITHNEOS Method: VIS


  23615 1996 FK12                     
        Warner 2015l                   A suspected 'wide binary'. The long period is the primary.
                                       The short period (U = 3) is for the fully asynchronous
                                       satellite.


  23621 1996 PA                       
        Binzel 2019                    MITHNEOS Method: sVIS


  23692 Nandatianwenners              
        Clark 2020                     Result of combining data from 2015 and 2019. The DateObs is
                                       the mid-date for the 2015 data set.

        Clark 2020                     Results table gives P = 9.315 h.


  23714 1998 EC3                      
        Binzel 2019                    MITHNEOS Method: TAXON


  23971 1998 YU9                      
        The Masi et al. paper gave this as a C-type on the basis of a netural spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  23983 1999 NS11                     
        Binzel 2019                    MITHNEOS Method: sVIS


  23998 1999 RP29                     
        Pravec 2019b                   Paired with (205383) 2001 BV47.


  24077 1999 TD233                    
        Warner 2014f                   Given periods may not be actual values, but linear
                                       combinations of the true NPAR periods.


  24445 2000 PM8                      
        Monteiro 2018b                 For all Monteiro 2018b: if the table date, period, and/or
                                       amplitude disagreed with the lightcurve, the value(s) in the
                                       plot were used.

        Binzel 2019                    MITHNEOS Method: VISNIR


  24475 2000 VN2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  24693 1990 SB2                      
        Binzel 2019                    MITHNEOS Method: sVIS


  24761 Ahau                          
        Binzel 2019                    MITHNEOS Method: sVISNIR


  24814 1994 VW1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  25021 Nischaykumar                  
        Pravec 2019b                   Paired with (453818) 2011 SJ109.


  25037 1998 QC37                     
        Binzel 2019                    MITHNEOS Method: sVIS


  25143 Itokawa                       
        Mueller 2011a                  H and G taken from other sources.

        Nishihara 2018                 Using all data from 2001-2004, P = 12.1324 h

        Binzel 2019                    MITHNEOS Method: VISNIR


  25330 1999 KV4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  25332 1999 KK6                      
        Warner 2013b                   Alternate suspected P2: 16.18 h.


  25362 1999 TH24                     
        Binzel 2019                    MITHNEOS Method: sVIS


  25884 Asai                          
        Pravec 2019b                   Paired with (48527) 1993 LC1.


  25916 2001 CP44                     
        Warner 2018m                   Period revised based on 2018 data/analysis.

        Binzel 2019                    MITHNEOS Method: VISNIR


  26093 1987 UA1                      
        Pravec 2012web                 Double period not formally excluded.


  26166 1995 QN3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  26209 1997 RD1                      
        Binzel 2019                    MITHNEOS Method: VIS


  26308 1998 SM165                    
        Brown 2002                     Sep ~ 6000 km


  26416 1999 XM84                     
        Pravec 2019b                   Paired with (214954) 2007 WO58.


  26420 1999 XL103                    
        Pravec 2019b                   Paired with 2012 TS209.


  26737 Adambradley                   
        Stephens 2020c                 Weak secondary period of 20-40 h noticeably improved the RMS
                                       for the 2.7 h solution.


  26760 2001 KP41                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  26858 Misterrogers                  
        Binzel 2019                    MITHNEOS Method: NIR


  26879 Haines                        
        Binzel 2019                    MITHNEOS Method: VIS


  27002 1998 DV9                      
        Binzel 2019                    MITHNEOS Method: TAXON


  27346 2000 DN8                      
        Binzel 2019                    MITHNEOS Method: NIR


  28736 2000 GE133                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  28913 2000 OT                       
        Behrend 2003web                Period originally reported as 15.30 h.


  29075 1950 DA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  29292 Conniewalker                  
        Pravec 2011web                 Several possible tumbling solutions.


  29407 1996 UW                       
        Binzel 2019                    MITHNEOS Method: sVIS


  30105 2000 FO3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  30301 Kuditipudi                    
        Pravec 2019b                   Paired with (205231) 2000 QY110.


  30717 1937 UD                       
        Binzel 2019                    MITHNEOS Method: sVIS


  30786 Karkoschka                    
        Binzel 2019                    MITHNEOS Method: sVIS


  30825 1990 TG1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  31210 1998 BX7                      
        Binzel 2019                    MITHNEOS Method: VIS


  31221 1998 BP26                     
        Binzel 2019                    MITHNEOS Method: TAXON


  31345 1998 PG                       
        Binzel 2019                    MITHNEOS Method: VIS


  31346 1998 PB1                      
        Binzel 2019                    MITHNEOS Method: VIS


  31367 1998 WB9                      
        Binzel 2019                    MITHNEOS Method: sVIS


  31415 1999 AK23                     
        Binzel 2019                    MITHNEOS Method: VIS


  31669 1999 JT6                      
        Binzel 2019                    MITHNEOS Method: NIR


  31832 2000 AP59                     
        Binzel 2019                    MITHNEOS Method: sVIS


  31843 2000 CQ80                     
        Binzel 2019                    MITHNEOS Method: sVIS


  31869 2000 EF101                    
        Binzel 2019                    MITHNEOS Method: sVIS


  32122 2000 LD10                     
        Binzel 2019                    MITHNEOS Method: sVIS


  32575 2001 QY78                     
        Binzel 2019                    MITHNEOS Method: sVIS


  32827 1992 DF1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  32897 Curtharris                    
        Binzel 2019                    MITHNEOS Method: sVIS


  32906 1994 RH                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  32957 1996 HX20                     
        Pravec 2019b                   Paired with (38707) 2000 QK89.


  33046 1997 UF2                      
        Pravec 2014web                 P2 not determined. One attenuations seen, but unexplained.


  33325 1998 RH3                      
        Pravec 2019b                   Paired with 2012 AX10.


  33342 1998 WT24                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  33881 2000 JK66                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  34048 2000 OR35                     
        Binzel 2019                    MITHNEOS Method: sVIS


  34613 2000 UR13                     
        Binzel 2019                    MITHNEOS Method: TAXON


  34755 2001 QW120                    
        Binzel 2019                    MITHNEOS Method: sVIS


  35107 1991 VH                       
        Merline 2008                   AO observations separated primary and satellite. Angular
                                       separation of 0.08' (~3.1 km). Satellite ~2.0 mag fainter.
                                       Separation and size agree with Pravec (IAUC 6607).

        Binzel 2019                    MITHNEOS Method: VISNIR


  35368 1997 UB8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  35396 1997 XF11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  35432 1998 BG9                      
        Binzel 2019                    MITHNEOS Method: VIS


  35670 1998 SU27                     
        Binzel 2019                    MITHNEOS Method: VIS


  35783 1999 JU20                     
        Warner 2022g                   Some suspicious secondary periods between 2-5 h, but the
                                       lightcurve amplitude and noise are about the same.


  36017 1999 ND43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  36183 1999 TX16                     
        Binzel 2019                    MITHNEOS Method: VIS


  36284 2000 DM8                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  37336 2001 RM                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  37384 2001 WU1                      
        Binzel 2019                    MITHNEOS Method: NIR


  37424 2001 YA3                      
        Benishek 2021k                 An unexplained attenuation may be due to third body.


  38071 1999 GU3                      
        Binzel 2019                    MITHNEOS Method: NIR


  38079 1999 HF                       
        Pravec 2020web                 The amplitudes for the Pravec 2020web observation subsets are
                                       for outside the mutual events.


  38086 Beowulf                       
        Binzel 2019                    MITHNEOS Method: TAXON


  38184 1999 KF                       
        Pravec 2019b                   Paired with (221867) 2008 GR80.


  38707 2000 QK89                     
        Pravec 2019b                   Paired with (32957) 1996 HX20.


  39235 2000 YH55                     
        Binzel 2019                    MITHNEOS Method: sVIS


  39489 1981 EU6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  39565 1992 SL                       
        Binzel 2019                    MITHNEOS Method: NIR


  39572 1993 DQ1                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  39702 1996 TZ10                     
        Binzel 2019                    MITHNEOS Method: sVIS


  40267 1999 GJ4                      
        Binzel 2019                    MITHNEOS Method: VIS


  40310 1999 KU4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  40366 1999 NF27                     
        Pravec 2019b                   Paired with (78024) 2002 JO70.


  42355 Typhon                        
        Noll 2006a                     Ds/Dp: ~0.5, assuming same albedo for both bodies.

        Grundy 2008                    Orbit SMA: 1628 ± 29 km. Ds: 84 ± 16 km.

        Benecchi 2009                  See note under 2001 QC298.


  42887 1999 RV155                    
        Binzel 2019                    MITHNEOS Method: sVIS


  42946 1999 TU95                     
        Pravec 2019b                   Paired with (165548) 2001 DO37.


  43008 1999 UD31                     
        Pravec 2019b                   Paired with (441549) 2008 TM68.


  43017 1999 VA2                      
        Binzel 2019                    MITHNEOS Method: sVIS


  44200 1998 MJ25                     
        Binzel 2019                    MITHNEOS Method: sVIS


  44534 1998 YZ9                      
        Polishook 2012b                Authors gave P=22.5 h but with monomodal solution. The
                                       amplitude virtually assures a bimodal lightcurve with a
                                       period about double the stated value.


  44612 1999 RP27                     
        Pravec 2012web                 Period assumed from work in 2010.

        Pravec 2012web                 Period assumed from work in 2010.

        Pravec 2019b                   Paired with (2210) Moore-Sitterly.


  44619 1999 RO42                     
        Binzel 2019                    MITHNEOS Method: sVIS


  44620 1999 RS43                     
        Pravec 2019b                   Paired with (295745) 2008 UH98.


  45251 1999 YN                       
        Binzel 2019                    MITHNEOS Method: sVIS


  45991 2001 BQ70                     
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  46162 2001 FM78                     
        Pravec 2019b                   Paired with (323879) 2004 SA204.


  46829 McMahon                       
        Pravec 2019b                   Paired with 2014 VR4. Observing Circumstances are for
                                       lightcurves from 2015 Feb.


  47035 1998 WS                       
        Binzel 2019                    MITHNEOS Method: VIS


  47171 Lempo                         
        Benecchi 2009                  See note under 2001 QC298.


  47581 2000 AN178                    
        Binzel 2019                    MITHNEOS Method: NIR


  47648 2000 CA40                     
        Binzel 2019                    MITHNEOS Method: sVIS


  48468 1991 SS1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  48527 1993 LC1                      
        Pravec 2019b                   Paired with (25884) Asai.


  48603 1995 BC2                      
        Binzel 2019                    MITHNEOS Method: VIS


  48621 1995 OC                       
        Binzel 2019                    MITHNEOS Method: sVIS


  48652 1995 VB                       
        Pravec 2019b                   Paired with (139156) 2001 FP106.


  49791 1999 XF31                     
        Pravec 2019b                   Paired with (436459) 2011 CL97.


  50000 Quaoar                        
        Fraser 2013                    Period is for a non-zero eccentric orbit. A solution near
                                       298.3 h is possible assuming a zero eccentricity.


  50867 2000 GM4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  51157 2000 HB57                     
        Binzel 2019                    MITHNEOS Method: sVIS


  51609 2001 HZ32                     
        Pravec 2019b                   Paired with (322672) 1999 TE221.


  51866 2001 PH3                      
        Pravec 2019b                   Paired with (326894) 2003 WV25.


  52340 1992 SY                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  52387 Huitzilopochtli               
        Binzel 2019                    MITHNEOS Method: NIR


  52750 1998 KK17                     
        Warner 2017c                   Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


  52760 1998 ML14                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


  52762 1998 MT24                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


  52768 1998 OR2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  52773 1998 QU12                     
        Pravec 2019b                   Paired with (279865) 2001 HU24.


  52852 1998 RB75                     
        Pravec 2019b                   Paired with (250322) 2003 SC7.


  53319 1999 JM8                      
        Binzel 2019                    MITHNEOS Method: sVISNIR

        Skiff 2019b                    Mid-date is approximate. Additional data from October also
                                       available.


  53430 1999 TY16                     
        Binzel 2019                    MITHNEOS Method: NIR


  53431 1999 UQ10                     
        Warner 2010k                   A weak signal with a period of 38.4 h was found. If this is
                                       subtracted from the data, the scatter in the data was reduced
                                       significantly. There was insufficent evidence to attribute
                                       the signal to a specific cause.


  53435 1999 VM40                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  53537 Zhangyun                      
        Pravec 2019b                   Paired with (503955) 2004 ED107.


  53576 2000 CS47                     
        Pravec 2019b                   Paired with ((421781) 2014 QG22.


  53789 2000 ED104                    
        Binzel 2019                    MITHNEOS Method: NIR


  54041 2000 GQ113                    
        Pravec 2019b                   Paired with (220143) 2002 TO134.


  54071 2000 GQ146                    
        Binzel 2019                    MITHNEOS Method: NIR


  54509 YORP                          
        Lowry 2007a                    Date for phase is end of period: Jul 28, 2001 - Jul 27, 2002.
                                       Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Aug. 12, 2004 - Aug. 31,
                                       2005. Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Jul 27, 2002 - Aug. 27,
                                       2003. Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Jul. 29, 2003 - Sep. 11,
                                       2004. Paper proved spin up due to YORP effect.

        Taylor 2007                    Date for phase is for beginning of observations that spanned
                                       from 2001 - 2005. Diameter and spin axis were determined from
                                       radar observations. Paper proved spin up due to YORP effect.
                                       

        Binzel 2019                    MITHNEOS Method: NIR


  54660 2000 UJ1                      
        Binzel 2019                    MITHNEOS Method: TAXON


  54686 2001 DU8                      
        Binzel 2019                    MITHNEOS Method: VIS


  54690 2001 EB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  54789 2001 MZ7                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2023a                   Secondary period lightcurve resembles one for a slightly
                                       elongated body, i.e., there is a possiblity that this is a
                                       'very wide binary.'


  54827 Kurpfalz                      
        Pravec 2010a                   Paired with (6070) Rheinland.

        Pravec 2019b                   Paired with (6070) Rheinland.


  55532 2001 WG2                      
        Stephens 2014e                 Unique solution not possible. Second period for NPAR table is
                                       one of several contenders.

        Binzel 2019                    MITHNEOS Method: VIS


  55576 Amycus                        
        Thirouin 2010                  Number given as 55567, which is 2002 CS6. The LCDB authors
                                       presumed the name/designation were correct.


  55764 1992 DG12                     
        Pravec 2019b                   Unspecified other possible periods. Paried with (305693) 2009
                                       BB131.


  55913 1998 FL12                     
        Pravec 2019b                   Paired with 2005 GQ107.


  56048 1998 XV39                     
        Pravec 2019b                   Paired with (76148) 2000 EP17.


  56150 1999 CT103                    
        Originally Derm4l in Dermawan Ph.D. thesis.


  56232 1999 JM31                     
        Pravec 2019b                   Paired with (115978) 2003 WQ56.


  56700 2000 LL28                     
        Pravec 2019b                   Paired with (414166) 2008 AU67.


  57047 2001 LG1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  57202 2001 QJ53                     
        Pravec 2019b                   Paired with (276353) 2002 UY20.


  58046 2002 XA14                     
        Binzel 2019                    MITHNEOS Method: sVIS


  59184 1999 AR15                     
        Pravec 2019b                   Paired with (293667) 2007 PD19.


  59394 1999 FZ23                     
        Pravec 2019b                   Paired with (11286) 1990 RO8.


  60458 2000 CM114                    
        Grundy 2019b                   For Grundy 2019b, the spin axis values are for the orbital
                                       pole. The primary's pole will be the same or similar.


  60546 2000 EE85                     
        Pravec 2019b                   Paired with (88604) 2001 QH293.


  60677 2000 GO18                     
        Pravec 2019b                   Paired with (142131) 2002 RV11.


  60735 2000 GF82                     
        Binzel 2019                    MITHNEOS Method: sVIS


  60744 2000 GB93                     
        Pravec 2019b                   Paired with (218099) 2002 MH3.


  60924 2000 JF44                     
        Binzel 2019                    MITHNEOS Method: sVIS


  61461 2000 QA31                     
        Warner 2011o                   One-night stand. Solution is based on a half-period analysis.


  61799 2000 QC184                    
        Binzel 2019                    MITHNEOS Method: sVIS


  63047 2000 WQ93                     
        Pravec 2019b                   Paired with (393274) 2013 WJ82.


  63095 2000 WS142                    
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


  63160 2000 YN8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  63164 2000 YU14                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  63291 2001 DU87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  63341 2001 FD77                     
        Binzel 2019                    MITHNEOS Method: sVIS


  63440 Rozek                         
        Pravec 2019b                   Paired with (331933) 2004 TV14.


  63583 2001 QP31                     
        Binzel 2019                    MITHNEOS Method: sVIS


  63970 2001 SG72                     
        Pravec 2019b                   Paired with 2013 CT63.


  65489 Ceto                          
        Benecchi 2009                  See note under 2001 QC298.


  65679 1989 UQ                       
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


  65706 1992 NA                       
        Binzel 2019                    MITHNEOS Method: VIS


  65733 1993 PC                       
        Binzel 2019                    MITHNEOS Method: NIR


  65784 Naderayama                    
        Binzel 2019                    MITHNEOS Method: NIR


  65803 Didymos                       
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Binzel 2019                    MITHNEOS Method: VISNIR


  65996 1998 MX5                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66008 1998 QH2                      
        Binzel 2019                    MITHNEOS Method: TAXON


  66063 1998 RO1                      
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Binzel 2019                    MITHNEOS Method: sVISNIR


  66146 1998 TU3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66251 1999 GJ2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66272 1999 JW6                      
        Warner 2021d                   A third period of P3 = 15.99 h is likely due to diurnal
                                       systematics. It has no effect on the P1/P2 solutions save to
                                       remove some noise from each lightcurve.


  66358 1999 JW87                     
        Binzel 2019                    MITHNEOS Method: sVIS


  66391 Moshup                        
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Behrend 2018web                Apparent mutual event on 2018 June 7 (UT) but not mentioned.

        Behrend 2018web                No signs of known satellite.

        Behrend 2019web                Phased curve shows known satellite mutual events. No
                                       secondary period reported.

        Binzel 2019                    MITHNEOS Method: NIR


  66419 1999 NR13                     
        Binzel 2019                    MITHNEOS Method: sVIS


  66652 Borasisi                      
        Noll 2004                      Alternate solution: P = 1109.6 Ãƒâ€šÃ‚Â± 1.6 h.

        Benecchi 2009                  See note under 2001 QC298.

        Grundy 2011                    Orbital period determined from astrometric measurements.


  66659 1999 TJ1                      
        Pravec 2019b                   Paired with (446085) 2013 CW179.


  66959 1999 XO35                     
        Binzel 2019                    MITHNEOS Method: VIS


  67399 2000 PJ6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  67502 2000 RE44                     
        Binzel 2019                    MITHNEOS Method: sVIS


  67729 2000 UQ23                     
        Binzel 2019                    MITHNEOS Method: sVIS


  67865 2000 WG23                     
        Binzel 2019                    MITHNEOS Method: VIS


  68063 2000 YJ66                     
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2022b                   An additional period of 5.73 h suggests a third body in the
                                       system.


  68216 2001 CV26                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Stephens 2015g                 No satellite found with radar observations in 2009.

        Binzel 2019                    MITHNEOS Method: VISNIR


  68278 2001 FC7                      
        Binzel 2019                    MITHNEOS Method: sVIS

        Pravec 2019web                 Unexplained deviations on 2018 Jan 14, 20, and 24.


  68346 2001 KZ66                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   YORP detection: (8.43 Ã‚Â± 0.69)*10^-8 rad/day/day. Combinded
                                       optical and radar data. Original optical raw data available
                                       at https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/.

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   Original raw lightcurve data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/


  68350 2001 MK3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  68359 2001 OZ13                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  68372 2001 PM9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  68548 2001 XR31                     
        Binzel 2019                    MITHNEOS Method: VIS


  68950 2002 QF15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  69142 2003 FL115                    
        Pravec 2019b                   Paired with (127502) 2002 TP59.


  69230 Hermes                        
        Binzel 2019                    MITHNEOS Method: NIR


  69298 1992 DR9                      
        Paired with 2012 FF11.


  69311 Russ                          
        Binzel 2019                    MITHNEOS Method: sVIS


  69406 Martz-Kohl                    
        Warner 2011k                   If the shorter period is correct, this makes the asteroid a
                                       good binary candidate.


  70030 Margaretmiller                
        Warner 2012b                   No mutual events seen but independent observations from two
                                       locations show a secondary period of either 15.8 or 11.5 h.


  70511 1999 TL103                    
        Pravec 2019b                   Paired with (462176) 2007 TC334.


  71997 2000 WD178                    
        Binzel 2019                    MITHNEOS Method: sVIS


  72204 2000 YV133                    
        Binzel 2019                    MITHNEOS Method: sVIS


  72748 2001 FR126                    
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


  73735 1993 QE3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  74096 1998 QD15                     
        Pravec 2019b                   Paired with (224857) 2006 YE45.


  74789 1999 SY5                      
        Binzel 2019                    MITHNEOS Method: sVIS


  76111 2000 DK106                    
        Pravec 2019b                   Paired with (354652) 2005 JY103.


  76148 2000 EP17                     
        Pravec 2019b                   Paired with (56048) 1998 XV39.


  76978 2001 BY60                     
        Binzel 2019                    MITHNEOS Method: sVIS


  77971 Donnolo                       
        Binzel 2019                    MITHNEOS Method: sVIS


  78024 2002 JO70                     
        Pravec 2019b                   Paired with (40366) 1999 NF 27.


  78085 2002 LV23                     
        Pravec 2023web                 Probably binary.  The solution for the two periods appears
                                       unique (but it is not clear which of them is the primary
                                       period).


  78587 2002 SZ12                     
        Binzel 2019                    MITHNEOS Method: sVIS


  79340 1996 TO41                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  79360 Sila-Nunam                    
        Benecchi 2009                  See note under 2001 QC298.


  79576 1998 QG98                     
        Binzel 2019                    MITHNEOS Method: sVIS


  80218 1999 VO123                    
        Pravec 2019b                   Paired with (213471) 2002 ES90.


  80806 2000 CM105                    
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is for the
                                       combined light since the binary pair could not be resolved.


  82075 2000 YW134                    
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is for the
                                       combined light since the binary pair could not be resolved.


  82105 2001 FG26                     
        Binzel 2019                    MITHNEOS Method: sVIS


  82676 2001 PV23                     
        Binzel 2019                    MITHNEOS Method: sVIS


  84203 2002 RD133                    
        Pravec 2019b                   Paired with (285637) 2000 SS4.


  85182 1991 AQ                       
        Binzel 2019                    MITHNEOS Method: TAXON


  85185 Lederman                      
        Binzel 2019                    MITHNEOS Method: sVIS


  85236 1993 KH                       
        Binzel 2019                    MITHNEOS Method: NIR


  85274 1994 GH                       
        Binzel 2019                    MITHNEOS Method: sVIS


  85275 1994 LY                       
        Binzel 2019                    MITHNEOS Method: NIR

        Masiero 2020b                  The geocentric phase angle and PAB in the Masiero 2020b
                                       details records were computed using the mean MJD given in the
                                       file. H-G are the values used for the model and appear only
                                       in details records. The MPCORB H-G at the time of import are
                                       used in the summary line. The albedo error is the larger
                                       linear error listed in the table. The diameter is the
                                       corrected value (see Masiero et al. 2020b).


  85490 1997 SE5                      
        Binzel 2019                    MITHNEOS Method: TAXON


  85585 Mjolnir                       
        Binzel 2019                    MITHNEOS Method: NIR


  85709 1998 SG36                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  85713 1998 SS49                     
        Binzel 2019                    MITHNEOS Method: NIR


  85770 1998 UP1                      
        Binzel 2019                    MITHNEOS Method: NIR


  85774 1998 UT18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  85804 1998 WQ5                      
        Binzel 2019                    MITHNEOS Method: NIR


  85818 1998 XM4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  85839 1998 YO4                      
        Binzel 2019                    MITHNEOS Method: NIR


  85848 1998 YP29                     
        Binzel 2019                    MITHNEOS Method: sVIS


  85867 1999 BY9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  85938 1999 DJ4                      
        Binzel 2019                    MITHNEOS Method: VIS


  85953 1999 FK21                     
        Binzel 2019                    MITHNEOS Method: VIS


  85989 1999 JD6                      
        Aznar 2018b                    Published lightcurve is inverted, i.e., faintest when at top.

        Binzel 2019                    MITHNEOS Method: VISNIR


  85990 1999 JV6                      
        Giorgini 2016                  Yarkovsky detection.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Giorgini 2019                  Yarkovsky detection. Replaces text in CBET 4279.

        Rozek 2019b                    Model is based on lightcurve/radar combination for a bilobed
                                       shape without a narrow 'neck.'


  86039 1999 NC43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  86067 1999 RM28                     
        Binzel 2019                    MITHNEOS Method: NIR


  86212 1999 TG21                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  86324 1999 WA2                      
        Binzel 2019                    MITHNEOS Method: NIR


  86326 1999 WK13                     
        Binzel 2019                    MITHNEOS Method: VIS


  86450 2000 CK33                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  86626 2000 EV124                    
        Binzel 2019                    MITHNEOS Method: sVIS


  86667 2000 FO10                     
        Binzel 2019                    MITHNEOS Method: NIR


  86819 2000 GK137                    
        Binzel 2019                    MITHNEOS Method: VISNIR


  86829 2000 GR146                    
        Binzel 2019                    MITHNEOS Method: VIS


  87024 2000 JS66                     
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2021web                 A2 amplitude assumed to be same as A1.

        Warner 2022c                   Third period: 39.46 Â± 0.01, A = 0.13 Â± 0.02. See Pravec et
                                       al. (2021web).


  87311 2000 QJ1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  87510 2000 QJ183                    
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


  87684 2000 SY2                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021a                   P2 is not a rotational alias of P1 and so the ambiguity lies
                                       in explaining the two periods. The low amplitudes and nearly
                                       the same periods precludes these being periods of a tumbler.
                                       


  87887 2000 SS286                    
        Pravec 2019b                   Paried with (415992) 2002 AT49.


  88188 2000 XH44                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021g                   Very wide binary candidate, but solution is very tenuous.


  88254 2001 FM129                    
        Binzel 2019                    MITHNEOS Method: VISNIR


  88259 2001 HJ7                      
        Pravec 2019b                   Paired with (337181) 1999 VA117.


  88604 2001 QH293                    
        Pravec 2019b                   Paired with (60546) 2000 EE85.


  88611 Teharonhiawako                
        Osip 2003                      Diameter is for primary if assuming density = 1.0 gcm^-3.
                                       Secondary diameter: 136 Ãƒâ€šÃ‚Â± 10 km.


  88666 2001 RP79                     
        Pravec 2019b                   Paired with (501710) 2014 UY23.


  88710 2001 SL9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  88938 2001 TR33                     
        Binzel 2019                    MITHNEOS Method: sVIS


  89136 2001 US16                     
        Binzel 2019                    MITHNEOS Method: VIS


  89355 2001 VS78                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  89766 2002 AO62                     
        Binzel 2019                    MITHNEOS Method: sVIS


  89830 2002 CE                       
        Binzel 2019                    MITHNEOS Method: VIS


  89958 2002 LY45                     
        Binzel 2019                    MITHNEOS Method: NIR


  90075 2002 VU94                     
        Binzel 2019                    MITHNEOS Method: NIR


  90367 2003 LC5                      
        Binzel 2019                    MITHNEOS Method: NIR


  90403 2003 YE45                     
        Binzel 2019                    MITHNEOS Method: NIR


  90416 2003 YK118                    
        Binzel 2019                    MITHNEOS Method: NIR


  90482 Orcus                         
        Brown 2010                     The stated diameter is the effecitve size of the Orcus-Vanth
                                       system. Individual diameters are 900 and 280 km, assuming the
                                       desnities and albedos are the same. If Vanth's albedo is 0.5
                                       that of Orcus, the diameters are 860 and 380 km.  The
                                       semi-major axis of the satellite orbit is 8980 ± 20 km.

        Sickafoose 2019                Diameter assumes a spherical shape.


  92336 2000 GY81                     
        Pravec 2019b                   Paired with (143662) 2003 SP84.


  92359 2000 HC24                     
        Binzel 2019                    MITHNEOS Method: sVIS


  93040 2000 SG                       
        Binzel 2019                    MITHNEOS Method: sVIS


  93751 2000 WH1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  94210 2001 BK33                     
        Binzel 2019                    MITHNEOS Method: sVIS


  95626 2002 GZ32                     
        Santos-Sanz 2020               Volume-equivalent diameter from 366x306x120 km.


  95711 2003 AK                       
        Pravec 2007web                 Period > 10h. 100 hr is one of several possible solutions.


  96011 2004 PD6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  96189 Pygmalion                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  96315 1997 AP10                     
        Binzel 2019                    MITHNEOS Method: NIR


  96562 1998 SZ138                    
        Binzel 2019                    MITHNEOS Method: sVIS


  96590 1998 XB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  97805 2000 OJ15                     
        Pravec 2019b                   Paired with (279230) 2009 UX122.


  98866 Giannabussolari               
        Pravec 2019b                   Paired with 2015 RV228.


  98891 2001 BK41                     
        Binzel 2019                    MITHNEOS Method: sVIS


  98943 2001 CC21                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2023e                   P1 = 5.0159 h is secure but requires subtracting two periods
                                       of unknown origin: P2 = 15.82(0.01), A2 = 1.30(0.03), P3 =
                                       11.26(0.02), A3 = 0.21(0.05)


  99248 2001 KY66                     
        Binzel 2019                    MITHNEOS Method: NIR


  99799 2002 LJ3                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  99869 2002 PF46                     
        Binzel 2019                    MITHNEOS Method: sVIS


  99907 1989 VA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  99913 1997 CZ5                      
        Binzel 2019                    MITHNEOS Method: VIS


  99935 2002 AV4                      
        Binzel 2019                    MITHNEOS Method: NIR


  99942 Apophis                       
        Licandro 2016b                 Diameter and albedo are the averages of the min/max values.

        Binzel 2019                    MITHNEOS Method: VISNIR


 100004 1983 VA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 100017 1989 TN2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 100085 1992 UY4                      
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: NIR


 100316 1995 MM2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 100440 1996 PJ6                      
        Pravec 2019b                   Paired with 2011 SE164.


 100480 1996 UK                       
        Binzel 2019                    MITHNEOS Method: VIS


 100553 Dariofo                       
        Binzel 2019                    MITHNEOS Method: sVIS


 100756 1998 FM5                      
        Binzel 2019                    MITHNEOS Method: VIS

        Warner 2022i                   Final solution required P3=2.54 h, A=0.08 mag. Periods 2 and
                                       3 are artifacts of additive multi-period analysis.


 100926 1998 MQ                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 101027 1998 QL71                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101065 1998 RV11                     
        Pravec 2019b                   Paired with (368313) 2002 PY103.


 101402 1998 VG1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101429 1998 VF31                     
        Binzel 2019                    MITHNEOS Method: NIR


 101554 1999 AL4                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101703 1999 CA150                    
        Pravec 2019b                   Paired with (142694) 2002 TW243.


 101742 1999 FO7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101811 1999 JQ6                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101818 1999 JD13                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101952 1999 RY31                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101955 Bennu                         
        Binzel 2019                    MITHNEOS Method: VISNIR


 102528 1999 US3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 102803 1999 VA169                    
        Binzel 2019                    MITHNEOS Method: sVIS


 103055 1999 XR134                    
        Pravec 2019b                   Paired with 2008 UZ220.


 103067 1999 XA143                    
        Binzel 2019                    MITHNEOS Method: NIR


 103501 2000 AT245                    
        Binzel 2019                    MITHNEOS Method: sVIS


 103506 2000 BD1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 103732 2000 CO103                    
        Binzel 2019                    MITHNEOS Method: sVIS


 104444 2000 GR3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 105155 2000 NG26                     
        Warner 2012g                   Many possible periods.


 105158 2000 OL                       
        Binzel 2019                    MITHNEOS Method: sVIS


 105247 2000 QH3                      
        Pravec 2019b                   Paired with 2009 SZ67.


 105943 2000 SY233                    
        Binzel 2019                    MITHNEOS Method: sVIS


 106589 2000 WN107                    
        Binzel 2019                    MITHNEOS Method: sVIS


 108182 2001 HY13                     
        Binzel 2019                    MITHNEOS Method: sVIS


 108410 2001 KG32                     
        Binzel 2019                    MITHNEOS Method: sVIS


 108519 2001 LF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 108522 2001 LQ                       
        Binzel 2019                    MITHNEOS Method: sVIS


 108663 2001 NE21                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 109077 2001 QR25                     
        Binzel 2019                    MITHNEOS Method: sVIS


 109226 2001 QH91                     
        Binzel 2019                    MITHNEOS Method: sVIS


 112221 2002 KH4                      
        Warner 2019p                   The binaries table gives P1 = 2.479 h and Ds/Dp >= 0.22. The
                                       P1 solution is extremely weak.


 112249 2002 LM9                      
        Pravec 2019b                   Paired with (261878) 2006 GR49.


 112985 2002 RS28                     
        Binzel 2019                    MITHNEOS Method: NIR


 114553 2003 BH42                     
        Binzel 2019                    MITHNEOS Method: sVIS


 114924 2003 QL41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 115978 2003 WQ56                     
        Pravec 2019b                   Paired with (56232) 1999 JM31.


 117306 2004 VF21                     
        Pravec 2019b                   Paired with (10123) Fideoja.


 118112 2665 T-3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 119067 2001 KP76                     
        Marchis 2008a                  No lightcurves per se. Hubble observations show a binary
                                       system with components about the same size separated by
                                       0'.29, or about 8200 km.


 119979 2002 WC19                     
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is the combined
                                       light since the binary pair could not be resolved.


 120347 Salacia                       
        Noll 2006e                     Satellite 2.3 mag fainter.

        Stansberry 2012                SMAxis of orbit: 5619 ± 87 km. Individual diameters: Primary:
                                       905 ± 103 km; Secondary: 303 ± 35 km.


 120352 Gordonwong                    
        Binzel 2019                    MITHNEOS Method: sVIS


 120450 1982 SV                       
        Binzel 2019                    MITHNEOS Method: sVIS


 120578 1995 QV12                     
        Warner 2014f                   Large zero-point offsets required to get period. Could be
                                       signs of tumbling.


 121210 1999 QG2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 122011 2000 GL28                     
        Originally Derm8f in Dermawan Ph.D. thesis.


 122173 2000 KC28                     
        Pravec 2019b                   Paired with (259585) 2003 UG220.


 122421 2000 QZ101                    
        Binzel 2019                    MITHNEOS Method: sVIS


 124146 2001 MQ12                     
        Binzel 2019                    MITHNEOS Method: sVIS


 124200 2001 OM81                     
        Binzel 2019                    MITHNEOS Method: sVIS


 125475 2001 WA15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 129493 1995 BM2                      
        Binzel 2019                    MITHNEOS Method: VIS


 129541 1996 PQ9                      
        Binzel 2019                    MITHNEOS Method: sVIS


 129737 1999 AA9                      
        Binzel 2019                    MITHNEOS Method: sVIS


 130778 2000 SX369                    
        Pravec 2015web                 Possible second period.


 131045 2000 YH32                     
        Binzel 2019                    MITHNEOS Method: VIS


 133027 2002 XJ4                      
        Binzel 2019                    MITHNEOS Method: sVIS


 133090 2003 MS9                      
        Michimani 2023                 Result using two data sets: 2021 Oct an 2021 Dec.


 133531 2003 TJ5                      
        Binzel 2019                    MITHNEOS Method: sVIS


 134340 Pluto                         
        Tholen 1997                    The diameter of 2700 km is the effective diameter of the
                                       Pluto/Charon system based on Pv and H.  Pluto: D = 2350 ± 50
                                       km.  Charon (primary satellite): D = 1250 ± 50 km  Nix
                                       (S/2005 P1): Sep: 48700 km. D ~ 46 km  Hydra (S/2005 P2): Sep
                                       64800 km. D ~ 61 km.


 134371 1995 RH                       
        Binzel 2019                    MITHNEOS Method: sVIS


 134422 1998 QM3                      
        Warner 2015d                   The periods are two of several sets of solutions.


 134509 1999 FC8                      
        Binzel 2019                    MITHNEOS Method: sVIS


 134860 2000 OJ67                     
        Benecchi 2009                  See note under 2001 QC298.


 136108 Haumea                        
        Lellouch 2010                  Visible and Thermal observations.

        Lockwood 2014                  Ellipsoid lengths: a = 960 km, b = 770 km, c = 495 km.

        Dunham 2019                    Diameter computed from volume of ellipsoid with (abc) =
                                       (1050,840,537) km.


 136472 Makemake                      
        Lim 2010                       A dark area has 0.02 < p_v < 0.12 and 310 < D_eff < 380 km.


 136564 1977 VA                       
        Binzel 2019                    MITHNEOS Method: NIR


 136582 1992 BA                       
        This note applies to all entries for Masiero et al. (2020a). The albedo error is the listed
        maximum possible value when converting albedo values from log space to value space. The
        phase angle in the details record is from the file since the actual date of observation was
        not given. The value for H is the 'model-out' value, which may differ slightly from the
        value used in the NEATM modeling (the value given in Tables 1-4). This maintains full
        agreement with the listed albedo and diameter. See Masiero et al. (2020a) for details about
        assumed errors in H and G.


 136617 1994 CC                       
        Brozovic 2009b                 Estimated sizes: S1 > 100 m; S2 > 5 m.

        Brozovic 2011                  Inner satellite: D = 113 ± 30 m. P = 26 ± 12 h. P_orb =
                                       29.832 ± 2.400 h.   Outer satellite: D = 80 ± 30m. P = 14 ±
                                       7h. P_orb = 201.024 ± 12.0 h.

        Binzel 2019                    MITHNEOS Method: VISNIR


 136618 1994 CN2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 136745 1995 WL8                      
        Binzel 2019                    MITHNEOS Method: VIS


 136770 1996 PC1                      
        Binzel 2019                    MITHNEOS Method: NIR


 136793 1997 AQ18                     
        Binzel 2019                    MITHNEOS Method: VIS


 136795 Tatsunokingo                  
        Binzel 2019                    MITHNEOS Method: VIS


 136818 Selqet                        
        Binzel 2019                    MITHNEOS Method: TAXON


 136839 1997 WT22                     
        The geocentric phase angle and PAB in the Masiero 2020b details records were computed using
        the mean MJD given in the file. H-G are the values used for the model and appear only in
        details records. The MPCORB H-G at the time of import are used in the summary line. The
        albedo error is the larger linear error listed in the table. The diameter is the corrected
        value (see Masiero et al. 2020b).


 136849 1998 CS1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 136923 1998 JH2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 136993 1998 ST49                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 137032 1998 UO1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 137052 Tjelvar                       
        Binzel 2019                    MITHNEOS Method: VIS


 137062 1998 WM                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 137064 1998 WP5                      
        Binzel 2019                    MITHNEOS Method: VIS


 137069 1998 WQ15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 137084 1998 XS16                     
        Binzel 2019                    MITHNEOS Method: NIR


 137125 1999 CT3                      
        Binzel 2019                    MITHNEOS Method: NIR


 137126 1999 CF9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 137158 1999 FB                       
        Binzel 2019                    MITHNEOS Method: VIS


 137170 1999 HF1                      
        Warner 2016n                   No indications of known satellite.

        Binzel 2019                    MITHNEOS Method: VISNIR


 137199 1999 KX4                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 137230 1999 RG22                     
        Binzel 2019                    MITHNEOS Method: sVIS


 137427 1999 TF211                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 137671 1999 XP35                     
        Binzel 2019                    MITHNEOS Method: NIR


 137799 1999 YB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 137805 1999 YK5                      
        Binzel 2019                    MITHNEOS Method: sVIS


 137924 2000 BD19                     
        Binzel 2019                    MITHNEOS Method: NIR


 137925 2000 BJ19                     
        Binzel 2019                    MITHNEOS Method: VIS


 138013 2000 CN101                    
        Binzel 2019                    MITHNEOS Method: sVIS


 138127 2000 EE14                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138131 2000 ES20                     
        Binzel 2019                    MITHNEOS Method: sVIS


 138155 2000 ES70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138175 2000 EE104                    
        Binzel 2019                    MITHNEOS Method: NIR


 138205 2000 EZ148                    
        Binzel 2019                    MITHNEOS Method: TAXON


 138258 2000 GD2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138325 2000 GO82                     
        Binzel 2019                    MITHNEOS Method: VIS


 138404 2000 HA24                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138524 2000 OJ8                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138846 2000 VJ61                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138852 2000 WN10                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138883 2000 YL29                     
        Binzel 2019                    MITHNEOS Method: NIR

        Skiff 2019b                    Lightcurve shape is similar to one produced by a satellite
                                       with mutual events. If so, Ds/Dp ~ 0.38.


 138893 2000 YH66                     
        Binzel 2019                    MITHNEOS Method: VIS


 138911 2001 AE2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138937 2001 BK16                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138947 2001 BA40                     
        Binzel 2019                    MITHNEOS Method: NIR


 138971 2001 CB21                     
        Period from Warner/Stephens is based on the combined data set. See independent entries in
        details tables for the two dates.

        Binzel 2019                    MITHNEOS Method: VIS

        Pravec 2022web                 Longer period is not formally excluded but is less likely.

        Warner 2022f                   Based on data from 2022 Feb 27 and 28


 139056 2001 FY                       
        Binzel 2019                    MITHNEOS Method: VIS


 139156 2001 FP106                    
        Pravec 2019b                   Paired with (48652) 1995 VB.


 139345 2001 KA67                     
        Stephens 2018j                 Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


 139359 2001 ME1                      
        Binzel 2019                    MITHNEOS Method: NIR


 139537 2001 QE25                     
        Pravec 2019b                   Paired with (210904) 2001 SR218.


 139622 2001 QQ142                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 139775 2001 QG298                    
        Lacerda 2011                   The paper presumes a 'contact binary.' However, the
                                       lightcurves presented do not show the obvious indicators of
                                       'shoulders' in the descending and ascending branches. The
                                       lightcurve can be equally explained by a simple,
                                       highly-elongated body.


 140039 2001 SO73                     
        Binzel 2019                    MITHNEOS Method: NIR


 141018 2001 WC47                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 141052 2001 XR1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 141079 2001 XS30                     
        Binzel 2019                    MITHNEOS Method: VIS


 141354 2002 AJ29                     
        Binzel 2019                    MITHNEOS Method: sVIS


 141424 2002 CD                       
        Binzel 2019                    MITHNEOS Method: NIR


 141432 2002 CQ11                     
        Binzel 2019                    MITHNEOS Method: NIR


 141484 2002 DB4                      
        Binzel 2019                    MITHNEOS Method: VIS


 141498 2002 EZ16                     
        Binzel 2019                    MITHNEOS Method: NIR


 141593 2002 HK12                     
        Binzel 2019                    MITHNEOS Method: NIR


 141670 2002 JS100                    
        Warner 2018a                   Period of 4.719 h cannot be formally excluded, but is not
                                       likely.


 142040 2002 QE15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 142131 2002 RV11                     
        Pravec 2019b                   Paired with (60677) 2000 GO18.


 142348 2002 RX211                    
        Binzel 2019                    MITHNEOS Method: NIR


 142464 2002 TC9                      
        Binzel 2019                    MITHNEOS Method: NIR


 142555 2002 TB58                     
        Binzel 2019                    MITHNEOS Method: VIS


 142561 2002 TX68                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 142694 2002 TW243                    
        Pravec 2019b                   Paired with (101703) 1999 CA150.


 142781 2002 UM11                     
        Warner 2014e                   Multiple solutions possible due to the nearly flat
                                       lightcurve.


 143381 2003 BC21                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 143487 2003 CR20                     
        Binzel 2019                    MITHNEOS Method: NIR


 143624 2003 HM16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 143651 2003 QO104                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 143662 2003 SP84                     
        Pravec 2019b                   Paired with (92336) 2000 GY81.


 143947 2003 YQ117                    
        Binzel 2019                    MITHNEOS Method: NIR


 144411 2004 EW9                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 144898 2004 VD17                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 144900 2004 VG64                     
        Binzel 2019                    MITHNEOS Method: NIR


 144901 2004 WG1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 144922 2005 CK38                     
        Binzel 2019                    MITHNEOS Method: NIR


 145656 4788 P-L                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 145720 1993 OX7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 147431 2003 JA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 148480 2001 FE155                    
        Binzel 2019                    MITHNEOS Method: sVIS


 148780 Altjira                       
        Grundy 2011                    Orbital period determined from astrometric measurements.


 149592 2004 CU51                     
        Binzel 2019                    MITHNEOS Method: sVIS


 150398 2000 EC59                     
        Originally Derm1e in Dermawan Ph.D. thesis.


 152558 1990 SA                       
        Binzel 2019                    MITHNEOS Method: NIR


 152560 1991 BN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 152563 1992 BF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 152627 1997 DF                       
        Binzel 2019                    MITHNEOS Method: NIR


 152637 1997 NC1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 152664 1998 FW4                      
        Binzel 2019                    MITHNEOS Method: NIR


 152679 1998 KU2                      
        Binzel 2019                    MITHNEOS Method: VIS


 152742 1998 XE12                     
        Binzel 2019                    MITHNEOS Method: TAXON


 152754 1999 GS6                      
        Binzel 2019                    MITHNEOS Method: NIR


 152756 1999 JV3                      
        Binzel 2019                    MITHNEOS Method: NIR


 152770 1999 RR28                     
        Binzel 2019                    MITHNEOS Method: NIR


 152858 1999 XN35                     
        Hills 2013b                    Several possible solutions for P_Orb, ranging from 11 to 36
                                       h, if the deviations are due to a satellite.


 152895 2000 CQ101                    
        Binzel 2019                    MITHNEOS Method: NIR


 152931 2000 EA107                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 152964 2000 GP82                     
        Binzel 2019                    MITHNEOS Method: sVIS


 152978 2000 GJ147                    
        Binzel 2019                    MITHNEOS Method: VIS


 153002 2000 JG5                      
        Binzel 2019                    MITHNEOS Method: VIS


 153201 2000 WO107                    
        Binzel 2019                    MITHNEOS Method: VIS


 153219 2000 YM29                     
        Binzel 2019                    MITHNEOS Method: NIR


 153591 2001 SN263                    
        Becker 2008                    Density (Primary): 1.2 ± 0.4 g/cm^3

        Nolan 2008                     Radar observations show three objects in the 2001 SN263
                                       system. Estimated sizes are 2 km, 1 km, and 0.400 km.

        Becker 2015b                   Dp: 2.5 ± 0.3 km; Ds1: 0.77 ± 0.12 km; Ds2: 0.43 ± 0.14 km.
                                       Porb1: 16.464 ± 0.048; Porb2: 150 ± 3 h.

        Binzel 2019                    MITHNEOS Method: sVISNIR


 153814 2001 WN5                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 153842 2001 XT30                     
        Binzel 2019                    MITHNEOS Method: NIR


 153953 2002 AD9                      
        Binzel 2019                    MITHNEOS Method: VIS


 153958 2002 AM31                     
        Binzel 2019                    MITHNEOS Method: TAXON


 154029 2002 CY46                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 154244 2002 KL6                      
        Binzel 2019                    MITHNEOS Method: NIR


 154276 2002 SY50                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 154278 2002 TB9                      
        Binzel 2019                    MITHNEOS Method: VIS


 154302 2002 UQ3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 154347 2002 XK4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 154453 2003 CJ11                     
        Binzel 2019                    MITHNEOS Method: NIR


 154555 2003 HA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 154634 2003 XX38                     
        Pravec 2019b                   Paired with (7343) Ockeghem.


 154715 2004 LB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 154828 2004 RT8                      
        Pravec 2019b                   Paired with (13284) 1998 QB52.


 155140 2005 UD                       
        Binzel 2019                    MITHNEOS Method: sVIS

        Huang 2021                     G is for G1. G2 = -0.006 Ãƒâ€šÃ‚Â± 0.006


 155334 2006 DZ169                    
        Binzel 2019                    MITHNEOS Method: sVISNIR


 156032 2001 RP142                    
        Binzel 2019                    MITHNEOS Method: sVIS


 156294 2001 WU66                     
        Chang 2021                     This note applies to all Chang 2021 (PSJ 2) entries. The
                                       observations were made in g and r2 bands. The photometric
                                       bands (for H) were assigned as SG and SR, respectively. The
                                       H_SR values were transformed to approximate V by using the
                                       LCDB V = SR+ 0.22. While not exact, this makes the values
                                       more compatible to H_V when plotting frequency-diameters. For
                                       diameter calculations, an albedo of 0.05 and G = 0.15 Ã‚Â±
                                       0.2 was assumed for both bands. Only some of the 53 objects
                                       could be tied to an object in the MPC database. For those
                                       without ID, and where possible, the phase and phase angle
                                       bisector values were assumed to be the same as for an
                                       identified object in the same observing block. The entries
                                       are flagged as being from a Sparse Wide-field Survey (SWF).


 157995 2000 LF26                     
        Binzel 2019                    MITHNEOS Method: sVIS


 158853 2004 NJ32                     
        Binzel 2019                    MITHNEOS Method: sVIS


 159111 2004 VG15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 159368 1979 QB                       
        Binzel 2019                    MITHNEOS Method: sVIS


 159402 1999 AP10                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 159493 2000 UA                       
        Binzel 2019                    MITHNEOS Method: NIR


 159533 2001 HH31                     
        Binzel 2019                    MITHNEOS Method: NIR


 159609 2002 AQ3                      
        Binzel 2019                    MITHNEOS Method: VIS


 159635 2002 CZ46                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 159857 2004 LJ1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 159882 2004 RQ289                    
        Binzel 2019                    MITHNEOS Method: sVIS


 159898 2004 TO216                    
        Binzel 2019                    MITHNEOS Method: sVIS


 160091 2000 OL67                     
        Marchis 2008a                  No lightcurve per se. Hubble observations show a binary
                                       system with the components separated by 0'.29, or about 7800
                                       km. The secondary was about 0.6m fainter than the primary.


 160092 2000 PL6                      
        Binzel 2019                    MITHNEOS Method: sVIS


 160137 2001 BU41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 160519 1995 CS3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 161989 Cacus                         
        Durech 2018a                   YORP detection.

        Binzel 2019                    MITHNEOS Method: NIR


 161998 1988 PA                       
        Franco 2011web                 Author gave P = 6.70 h for a monomodal solution. The
                                       amplitude virtually assures a bimodal curve and, therefore,
                                       double the reported period.

        Binzel 2019                    MITHNEOS Method: sVISNIR


 162000 1990 OS                       
        Binzel 2019                    MITHNEOS Method: VIS


 162011 Konnohmaru                    
        Binzel 2019                    MITHNEOS Method: VIS


 162015 1994 TF2                      
        Binzel 2019                    MITHNEOS Method: VIS


 162038 1996 DH                       
        Binzel 2019                    MITHNEOS Method: sVIS


 162058 1997 AE12                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162117 1998 SD15                     
        Binzel 2019                    MITHNEOS Method: NIR


 162142 1998 VR                       
        Binzel 2019                    MITHNEOS Method: VIS


 162149 1998 YQ11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162157 1999 CV8                      
        Binzel 2019                    MITHNEOS Method: VIS


 162173 Ryugu                         
        Binzel 2019                    MITHNEOS Method: VISNIR

        Watanabe 2019                  Diameter is equatorial. Polar is 872 m. Spherical equivalent
                                       is D = 0.955 km.


 162181 1999 LF6                      
        Binzel 2019                    MITHNEOS Method: NIR


 162186 1999 OP3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 162361 2000 AF6                      
        Warner 2019m                   The solution for the secondary period (14.654 h) is very weak
                                       but its subtraction significantly lowers the RMS of the fit
                                       for the primary period.


 162385 2000 BM19                     
        Binzel 2019                    MITHNEOS Method: VIS


 162421 2000 ET70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 162422 2000 EV70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 162483 2000 PJ5                      
        Polishook 2008a                P_orb = 56.6 h is also possible.

        Binzel 2019                    MITHNEOS Method: VISNIR


 162510 2000 QW69                     
        The albedo error given for Masiero 2017 is the maximum possible value when converting from
        albedo values from log space to value space.


 162566 2000 RJ34                     
        Binzel 2019                    MITHNEOS Method: NIR


 162567 2000 RW37                     
        Binzel 2019                    MITHNEOS Method: VIS


 162581 2000 SA10                     
        Binzel 2019                    MITHNEOS Method: NIR


 162635 2000 SS164                    
        Binzel 2019                    MITHNEOS Method: NIR


 162740 2000 WF6                      
        Binzel 2019                    MITHNEOS Method: VIS


 162781 2000 XL44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162785 2000 YA17                     
        Binzel 2019                    MITHNEOS Method: sVIS


 162900 2001 HG31                     
        Pravec 2008web                 Pravec analysis based on data from Warner 2009f and from
                                       Lowell Observatory (unpublished).

        Binzel 2019                    MITHNEOS Method: NIR


 162903 2001 JV2                      
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 162911 2001 LL5                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 162998 2001 SK162                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 163000 2001 SW169                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 163001 2001 SE170                    
        Binzel 2019                    MITHNEOS Method: NIR


 163014 2001 UA5                      
        Binzel 2019                    MITHNEOS Method: VIS


 163081 2002 AG29                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163132 2002 CU11                     
        Binzel 2019                    MITHNEOS Method: NIR


 163191 2002 EQ9                      
        Binzel 2019                    MITHNEOS Method: NIR


 163243 2002 FB3                      
        Binzel 2019                    MITHNEOS Method: NIR


 163249 2002 GT                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 163250 2002 GH1                      
        Binzel 2019                    MITHNEOS Method: NIR


 163364 2002 OD20                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163468 2002 RZ177                    
        Warner 2023f                   Peirod derived from a best-fit of the half-period.


 163692 2003 CY18                     
        Binzel 2019                    MITHNEOS Method: sVIS

        Warner 2022i                   Periods 2 and 3 are artifacts of additive multi-period
                                       analysis.


 163693 Atira                         
        Rivera-Valentin 2017           Diameter is that estimated for the primary. The satellite
                                       diameter is 1.0 ±0.3 km

        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       45.2-97.3 deg. The H_SR values are the linear extrapolation
                                       using the phase slope (beta_SR) of 0.03584. The lack of low
                                       phase angles prevented use of H-G or HG1,G2 modeling.


 163697 2003 EF54                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163732 2003 KP2                      
        Binzel 2019                    MITHNEOS Method: VIS


 163899 2003 SD220                    
        Binzel 2019                    MITHNEOS Method: NIR

        Bondarenko 2019b               Diameter is for an effective spherical shape based on
                                       2700x1100 m a/b axis estimates.


 164121 2003 YT1                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: NIR


 164184 2004 BF68                     
        Binzel 2019                    MITHNEOS Method: TAXON


 164202 2004 EW                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 164206 2004 FN18                     
        Binzel 2019                    MITHNEOS Method: NIR


 164211 2004 JA27                     
        Binzel 2019                    MITHNEOS Method: NIR


 164214 2004 LZ11                     
        Binzel 2019                    MITHNEOS Method: sVIS


 164222 2004 RN9                      
        Binzel 2019                    MITHNEOS Method: NIR


 164400 2005 GN59                     
        Binzel 2019                    MITHNEOS Method: NIR


 164670 1996 XM6                      
        Binzel 2019                    MITHNEOS Method: NIR


 165389 2000 WC188                    
        Pravec 2019b                   Paired with 2011 SE164.


 165394 2000 XC15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 165548 2001 DO37                     
        Pravec 2019b                   Paired with (42946) 1999 TU95. Observing Circumstances for
                                       when Sloan color measurements from Lowell Observatory were
                                       made.


 167405 2003 WP118                    
        Pravec 2019b                   Paired with 2012 TK84.


 168315 1982 RA1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 168378 1997 ET30                     
        Binzel 2019                    MITHNEOS Method: NIR


 168710 2000 HE41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 168889 2000 WM95                     
        Binzel 2019                    MITHNEOS Method: VIS


 169660 2002 JG66                     
        Binzel 2019                    MITHNEOS Method: sVIS


 169675 2002 JM97                     
        Binzel 2019                    MITHNEOS Method: NIR


 170086 2002 XR14                     
        Binzel 2019                    MITHNEOS Method: NIR


 170172 2003 HV7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 170502 2003 WM7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 170880 2004 PH85                     
        Binzel 2019                    MITHNEOS Method: sVIS


 170891 2004 TY16                     
        Binzel 2019                    MITHNEOS Method: NIR


 171677 2000 QG136                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 224 = 2000 QG136. TALCS 1238 = 171677.


 171730 2000 WX50                     
        Binzel 2019                    MITHNEOS Method: NIR


 171784 2001 BV67                     
        Binzel 2019                    MITHNEOS Method: sVIS


 171839 2001 JM1                      
        Binzel 2019                    MITHNEOS Method: VIS


 172678 2003 YM137                    
        Binzel 2019                    MITHNEOS Method: VIS


 173154 1996 ME                       
        Binzel 2019                    MITHNEOS Method: sVIS


 173689 2001 PK9                      
        Binzel 2019                    MITHNEOS Method: NIR


 173885 2001 UA61                     
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 158 = 2001 UA61. TALCS 1699 = 173885.


 173974 2001 XV127                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 200 = 2001 VV127. TALCS 1054 = 173974.


 173991 2001 XR170                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 249 = 2001 XR170. TALCS 2205 = 173991.


 174567 Varda                         
        Grundy 2015                    Periods are based on Orbit1 solution. Diameters: Varda 722 ±
                                       82; Ilmare 326 ± 38.


 175047 2004 FK93                     
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 152 = 2004 FK93. TALCS 1699 = 175047.


 175706 1996 FG3                      
        Scheirich 2009                 Satellite:primary size ratio (D2/D1): 0.28 ± 0.02.
                                       Orbit:primary diameter ratio (a/A1): 3.1 ± 0.9.

        Mueller 2011a                  H and G taken from other sources.

        Wolters 2011                   D_sat = 0.51 0.03, assuming the same albedo as the primary.

        Scheirich 2015                 Data covered multipl apparitions from 1999-2013.

        Binzel 2019                    MITHNEOS Method: VISNIR


 175729 1998 BB10                     
        Binzel 2019                    MITHNEOS Method: VIS


 177255 2003 WC25                     
        Binzel 2019                    MITHNEOS Method: sVIS


 179806 2002 TD66                     
        Binzel 2019                    MITHNEOS Method: TAXON


 180186 2003 QZ30                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 181563 2006 UQ329                    
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


 181882 1999 RF14                     
        The given period is for an obvious short-term period in the raw data, which - on the whole -
        show a steady brightening over the observations. This could either be a tumbler or a very
        wide binary.

        Skiff 2023                     The given period is for an obvious short-term period in the
                                       raw data, which - on the whole - show a steady brightening
                                       over the observations. This could either be a tumbler or a
                                       very wide binary.


 182259 2001 FZ185                    
        Pravec 2019b                   Paired with (289y) Ole Romer.


 184266 2004 VW14                     
        Binzel 2019                    MITHNEOS Method: NIR


 184990 2006 KE89                     
        Warner 2020j                   The 2+ rating is a combination of a U=2 for the primary and
                                       U=3 for the secondary period.


 185851 2000 DP107                    
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Margot 2000                    Estimated diameters: 800 m and 300 m.

        Ostro 2000b                    Radar images show separations up to at least 1 km between
                                       components.

        Pravec 2000e                   Lightcurve observations confirmed binary nature discovered by
                                       radar.

        Scheirich 2009                 Solution 1: Satellite:primary size ratio (D2/D1): 0.43 ± 0.3.
                                       Orbit:primary diameter ratio (a/A1): 5.0 ± 2.0. Orbit period
                                       (sidereal): 42.09 ± 0.13  Solution 2: Satellite:primary size
                                       ratio (D2/D1): 0.43 ± 0.2. Orbit:primary diameter ratio
                                       (a/A1): 4.9 ± 1.2. Orbit period (sidereal): 42.79 ± 0.11

        Binzel 2019                    MITHNEOS Method: NIR


 187026 2005 EK70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 187737 2153 P-L                      
        Binzel 2019                    MITHNEOS Method: sVIS


 188452 2004 HE62                     
        Binzel 2019                    MITHNEOS Method: NIR


 189040 2000 MU1                      
        Binzel 2019                    MITHNEOS Method: VIS


 189494 1999 YY3                      
        Binzel 2019                    MITHNEOS Method: VIS


 189552 2000 RL77                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 190208 2006 AQ                       
        Warner 2015g                   No events seen and not likely so because of the long second
                                       period. The long period is attributed to the primary body
                                       while the short period is presumed to be due to the rotation
                                       of the fully asynchronous satellite.

        Binzel 2019                    MITHNEOS Method: NIR


 190491 2000 FJ10                     
        Binzel 2019                    MITHNEOS Method: VIS


 192559 1998 VO                       
        Binzel 2019                    MITHNEOS Method: TAXON


 192563 1998 WZ6                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 194006 2001 SG10                     
        Binzel 2019                    MITHNEOS Method: VIS


 194268 2001 UY4                      
        Binzel 2019                    MITHNEOS Method: VIS


 194386 2001 VG5                      
        Binzel 2019                    MITHNEOS Method: VIS


 196299 2003 FN1                      
        Binzel 2019                    MITHNEOS Method: NIR


 197994 2004 RG165                    
        Binzel 2019                    MITHNEOS Method: NIR


 198856 2005 LR3                      
        Binzel 2019                    MITHNEOS Method: NIR


 199003 2005 WJ56                     
        Binzel 2019                    MITHNEOS Method: NIR


 200754 2001 WA25                     
        Binzel 2019                    MITHNEOS Method: VIS


 200840 2001 XN254                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 202079 2004 SR39                     
        Binzel 2019                    MITHNEOS Method: sVIS


 203015 1999 YF3                      
        Binzel 2019                    MITHNEOS Method: VIS


 203471 2002 AU4                      
        Binzel 2019                    MITHNEOS Method: NIR


 203489 2002 AL80                     
        Pravec 2019b                   Paired with (17288) 2000 NZ10.


 205231 2000 QY110                    
        Pravec 2019b                   Paired with (30301) Kuditipudi.


 205383 2001 BV47                     
        Pravec 2019b                   Paired with (23998) 1999 RP29.


 205640 2001 XQ4                      
        Binzel 2019                    MITHNEOS Method: NIR


 205698 Troiani                       
        Binzel 2019                    MITHNEOS Method: NIR


 205744 2002 BK25                     
        Binzel 2019                    MITHNEOS Method: VIS


 206910 2004 NL8                      
        Binzel 2019                    MITHNEOS Method: NIR


 207398 2006 AS2                      
        Binzel 2019                    MITHNEOS Method: TAXON


 207408 2006 BY172                    
        Binzel 2019                    MITHNEOS Method: NIR


 207945 1991 JW                       
        Binzel 2019                    MITHNEOS Method: NIR


 207970 1996 BZ3                      
        Binzel 2019                    MITHNEOS Method: VIS


 208023 1999 AQ10                     
        Binzel 2019                    MITHNEOS Method: TAXON


 210482 1996 RW1                      
        Binzel 2019                    MITHNEOS Method: VIS


 210904 2001 SR218                    
        Pravec 2019b                   Paired with (139537) 2001 QE25.


 213084 1999 TN169                    
        Binzel 2019                    MITHNEOS Method: sVIS


 213471 2002 ES90                     
        Pravec 2019b                   Paired with (80218) 1999 VO123.


 214088 2004 JN13                     
        Warner 2015h                   Period forced to solution derived from 2014 December
                                       observations by Warner.

        Binzel 2019                    MITHNEOS Method: NIR


 214869 2007 PA8                      
        Lin 2018                       Additional observations in 2013 Jan were at much larger phase
                                       angles. Phase reddening may have affected the final result.

        Binzel 2019                    MITHNEOS Method: VISNIR


 214954 2007 WO58                     
        Pravec 2019b                   Paired with (26416) 1999 XM84.


 215188 2000 NM                       
        Binzel 2019                    MITHNEOS Method: TAXON


 216202 2006 UJ13                     
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


 216722 2005 EC286                    
        Binzel 2019                    MITHNEOS Method: sVIS


 217390 2005 CW25                     
        Binzel 2019                    MITHNEOS Method: TAXON


 217796 2000 TO64                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 217807 2000 XK44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 218099 2002 MH3                      
        Pravec 2019b                   Paired with (60744) 2000 GB93.


 218144 2002 RL66                     
        Warner 2010e                   The short period, low amplitude component of the lightcurve
                                       may be due to a widely separated component of a binary that
                                       is a relatively small and irregularly shaped, or a larger but
                                       more regularly shaped body.   If a binary, the period of the
                                       orbit cannot be determined from the observations but is
                                       probably long based on the absence of mutual events and
                                       asynchronous rotation of the two components.  The
                                       low-amplitude component of the lightcurve is U = 1/1+. This
                                       applies not only to the quality of the solution for the
                                       component but to the probability of the asteroid being binary
                                       as well.

        Warner 2010m                   The assignment of primary and secondary in this system is
                                       arbitrary.


 218863 2006 WO127                    
        Binzel 2019                    MITHNEOS Method: NIR


 219071 1997 US9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 219523 2001 QS84                     
        Binzel 2019                    MITHNEOS Method: sVIS


 220124 2002 TE66                     
        Binzel 2019                    MITHNEOS Method: NIR


 221867 2008 GR90                     
        Pravec 2019b                   Paired with (38184) 1999 KF.


 222165 2000 AX93                     
        Binzel 2019                    MITHNEOS Method: VIS


 224857 2006 YE45                     
        Pravec 2019b                   Paired with (74096) 1998 QD115.


 226268 2003 AN55                     
        Pravec 2019b                   Paired with (409156) 2003 UW156.


 228368 2000 WK10                     
        Binzel 2019                    MITHNEOS Method: VIS


 229007 2003 XF11                     
        Binzel 2019                    MITHNEOS Method: NIR


 229056 2004 FC126                    
        Pravec 2019b                   Paired with (17198) Gorjup.


 229401 2005 SU152                    
        Pravec 2019b                   Paired with 2004 UY97.


 229762 G||'homdima                   
        Grundy 2019a                   Effective diameter for primary body. Satellite diameter: 142
                                       Ãƒâ€šÃ‚Â± 8 km.


 230111 2001 BE10                     
        Binzel 2019                    MITHNEOS Method: NIR


 230979 2005 AT42                     
        Binzel 2019                    MITHNEOS Method: NIR


 231134 2005 TU45                     
        Binzel 2019                    MITHNEOS Method: NIR


 231937 2001 FO32                     
        Binzel 2019                    MITHNEOS Method: NIR


 232691 2004 AR1                      
        Binzel 2019                    MITHNEOS Method: NIR


 233401 2006 FF39                     
        Pravec 2019b                   Paired with (180856) 2005 HX5.


 234061 1999 HE1                      
        Binzel 2019                    MITHNEOS Method: NIR


 234145 2000 EW70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 235756 2004 VC                       
        Binzel 2019                    MITHNEOS Method: NIR


 236716 2007 FV42                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 237442 1999 TA10                     
        Binzel 2019                    MITHNEOS Method: NIR


 238063 2003 EG                       
        Binzel 2019                    MITHNEOS Method: VIS


 241662 2000 KO44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 241676 2000 QW158                    
        Binzel 2019                    MITHNEOS Method: NIR


 242187 2003 KR18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 242643 2005 NZ6                      
        Binzel 2019                    MITHNEOS Method: NIR


 243025 2006 UM216                    
        Warner 2020c                   A secondary period could not be found.


 244977 2004 BE68                     
        Binzel 2019                    MITHNEOS Method: NIR


 247517 2002 QY6                      
        Binzel 2019                    MITHNEOS Method: NIR


 248083 2004 QU24                     
        Binzel 2019                    MITHNEOS Method: NIR


 248818 2006 SZ217                    
        Binzel 2019                    MITHNEOS Method: NIR


 250112 2002 KY14                     
        Also designated 2007 UL126.


 250322 2003 SC7                      
        Pravec 2019b                   Paired with (52852) 1998 RB75.


 251346 2007 SJ                       
        Binzel 2019                    MITHNEOS Method: NIR


 252399 2001 TX44                     
        Binzel 2019                    MITHNEOS Method: NIR


 252793 2002 FW5                      
        Warner 2017i                   Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


 253062 2002 TC70                     
        Binzel 2019                    MITHNEOS Method: VIS


 253841 2003 YG118                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 256412 2007 BT2                      
        Binzel 2019                    MITHNEOS Method: NIR


 257744 2000 AD205                    
        Binzel 2019                    MITHNEOS Method: NIR


 257838 2000 JQ66                     
        Binzel 2019                    MITHNEOS Method: VIS


 258640 2002 ER36                     
        Pravec 2019b                   Paired with (1741) Giclas.


 259585 2003 UG220                    
        Pravec 2019b                   Paired with (122173) 2000 KC28.


 260141 2004 QT24                     
        Binzel 2019                    MITHNEOS Method: NIR


 261878 2006 GR49                     
        Pravec 2019b                   Paired with (112249) 2002 LM9.


 262623 2006 WY2                      
        Binzel 2019                    MITHNEOS Method: NIR


 263976 2009 KD5                      
        Binzel 2019                    MITHNEOS Method: TAXON


 264308 1999 NA5                      
        Binzel 2019                    MITHNEOS Method: NIR


 264357 2000 AZ93                     
        Binzel 2019                    MITHNEOS Method: NIR


 265187 2003 YS117                    
        Binzel 2019                    MITHNEOS Method: NIR


 267182 2000 QX57                     
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


 267494 2002 JB9                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 267729 2003 FC5                      
        Binzel 2019                    MITHNEOS Method: NIR


 269690 1996 RG3                      
        Binzel 2019                    MITHNEOS Method: NIR


 274138 2008 FU6                      
        Binzel 2019                    MITHNEOS Method: NIR


 274855 2009 RB4                      
        Binzel 2019                    MITHNEOS Method: NIR


 275677 2000 RS11                     
        Warner 2014i                   This entry is for the combined plot from 2014 March 16 and
                                       17.

        Binzel 2019                    MITHNEOS Method: VIS


 275792 2001 QH142                    
        Binzel 2019                    MITHNEOS Method: NIR


 276049 2002 CE26                     
        Warner 2015g                   Using either P1 = 3.088 or 3.298 (found by Pravec et al.,
                                       2006) produces the same period and lightcurve for P2.

        Binzel 2019                    MITHNEOS Method: NIR


 276353 2002 UY20                     
        Pravec 2019b                   Paired with (57202) 2001 QJ53.


 276397 2002 XA40                     
        Binzel 2019                    MITHNEOS Method: NIR


 276400 2002 XS45                     
        Binzel 2019                    MITHNEOS Method: TAXON


 276741 2004 EM66                     
        Binzel 2019                    MITHNEOS Method: NIR


 276770 2004 HC                       
        Binzel 2019                    MITHNEOS Method: NIR


 277127 2005 GW119                    
        Binzel 2019                    MITHNEOS Method: NIR


 277475 2005 WK4                      
        Binzel 2019                    MITHNEOS Method: NIR


 278067 2006 YY40                     
        Pravec 2019b                   Paired with (19289) 1996 HY12.


 279230 2009 UX122                    
        Pravec 2019b                   Paired with (97805) 2000 OJ15.


 279744 1998 KM3                      
        Binzel 2019                    MITHNEOS Method: NIR


 279865 2001 HU24                     
        Pravec 2019b                   Paired with (52773) 1998 QU12.


 282206 2001 VN61                     
        Pravec 2019b                   Paired with (165389) 2000 WC188.


 283319 1992 WR4                      
        Binzel 2019                    MITHNEOS Method: NIR


 283377 2000 PO9                      
        Binzel 2019                    MITHNEOS Method: NIR


 283457 2001 MQ3                      
        Binzel 2019                    MITHNEOS Method: NIR


 283460 2001 PD1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 283827 2003 TP15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 285263 1998 QE2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 285540 2000 GU127                    
        Binzel 2019                    MITHNEOS Method: VIS


 285631 2000 RB84                     
        Binzel 2019                    MITHNEOS Method: sVIS


 285637 2000 SS4                      
        Pravec 2019b                   Paired with (84203) 2002 RD1333.


 285838 2001 FA1                      
        Binzel 2019                    MITHNEOS Method: NIR


 289315 2005 AN26                     
        Binzel 2019                    MITHNEOS Method: NIR


 291188 2006 AL54                     
        Pravec 2019b                   Paired with (15107) Toepperwein.


 293667 2007 PD19                     
        Pravec 2019b                   Paired with (59184) 1999 AR15.


 295745 2008 UH98                     
        Pravec 2019b                   Paired with (44620) 1999 RS43.


 297274 1996 SK                       
        Binzel 2019                    MITHNEOS Method: NIR


 297418 2000 SP43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 301844 1990 UA                       
        Binzel 2019                    MITHNEOS Method: NIR


 301964 2000 EJ37                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 302311 2002 AA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 302831 2003 FH                       
        Binzel 2019                    MITHNEOS Method: NIR


 303174 2004 FH11                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 303712 2005 PR21                     
        Noll 2008d                     No lightcurve observations per se. Two components separated
                                       by 0'.123 ± 0'.009, or about 4000 km. Secondary component
                                       about 1.1 mag fainter than primary.


 305693 2009 BB131                    
        Pravec 2019b                   Paired with (55764) 1992 DG12.


 306376 1983 TA                       
        Binzel 2019                    MITHNEOS Method: NIR


 306453 1999 BE8                      
        Binzel 2019                    MITHNEOS Method: NIR


 306459 1999 GS3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 306895 2001 TT127                    
        Binzel 2019                    MITHNEOS Method: NIR


 307005 2001 XP1                      
        Binzel 2019                    MITHNEOS Method: NIR


 307070 2002 AV31                     
        Binzel 2019                    MITHNEOS Method: NIR


 307161 2002 DY3                      
        Binzel 2019                    MITHNEOS Method: VIS


 307556 2003 EQ43                     
        Binzel 2019                    MITHNEOS Method: sVIS


 307566 2003 FK22                     
        Binzel 2019                    MITHNEOS Method: NIR


 308020 2004 RM222                    
        Binzel 2019                    MITHNEOS Method: sVIS


 308127 2004 XM130                    
        This note applies to all entries for Masiero et al. (2021; Plan. Sci. J. 2, A162). The
        albedo error is the listed maximum possible value when converting albedo values from log
        space to value space. The phase angle in the details record is from the file since the
        actual date of observation was not given. The value for H is the 'model-out' value, which
        may differ slightly from the value used in the NEATM modeling (the value given in Tables
        1-4). This maintains full agreement with the listed albedo and diameter. No specific errors
        for H and G were given. Default values of H_err = 0.05 and G_err = 0.1 were used.


 308635 2005 YU55                     
        Bodewits 2011                  H_V was derived from UV observations that gave H_UV = 25.6.

        Merline 2012                   a = 337 ± 14 m; b = 326 ± 8 m; c = 263 ± 12 m.

        Binzel 2019                    MITHNEOS Method: VISNIR


 309214 2007 LL                       
        Binzel 2019                    MITHNEOS Method: NIR


 309662 2008 EE                       
        Binzel 2019                    MITHNEOS Method: NIR


 310226 2011 SU230                    
        Masiero 2009                   Also identified as 2005 ED209 during the TALCS survey.


 310402 1999 EE5                      
        Binzel 2019                    MITHNEOS Method: VIS


 310429 1999 XP19                     
        Binzel 2019                    MITHNEOS Method: sVIS


 310442 2000 CH59                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 310560 2001 QL142                    
        Pravec 2019web                 Attenuations seen but a consistent secondary period could not
                                       be found.


 311066 2004 DC                       
        Taylor 2006                    Ds ~ 0.060 km.


 311925 2007 BF72                     
        Binzel 2019                    MITHNEOS Method: VIS


 312473 2008 SX245                    
        Binzel 2019                    MITHNEOS Method: sVISNIR


 312497 2009 BR60                     
        Pravec 2019b                   Paired with (3749) Balam.


 313538 2002 YB12                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 313591 2003 MB7                      
        Binzel 2019                    MITHNEOS Method: NIR


 313701 2003 UN3                      
        Pravec 2019b                   Paired with 2012 KL9.


 316651 1990 OL                       
        Binzel 2019                    MITHNEOS Method: sVIS


 316720 1998 BE7                      
        Binzel 2019                    MITHNEOS Method: NIR


 316876 2000 RF43                     
        Binzel 2019                    MITHNEOS Method: sVIS


 316934 2001 AA52                     
        Binzel 2019                    MITHNEOS Method: NIR


 320378 2007 UR3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 321651 2010 BY9                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 322386 2011 QY34                     
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 322652 1999 JO8                      
        Binzel 2019                    MITHNEOS Method: VIS


 322672 1999 TE221                    
        Pravec 2019b                   Paired with (51609) 2001 HZ32.


 322775 2001 HA8                      
        Binzel 2019                    MITHNEOS Method: VIS


 323879 2005 SA204                    
        Pravec 2019b                   Paired with (46162) 2001 FM78.


 325769 2010 LY63                     
        Binzel 2019                    MITHNEOS Method: NIR


 326290 Akhenaten                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 326350 2000 SS217                    
        Binzel 2019                    MITHNEOS Method: sVIS


 326732 2003 HB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 326894 2003 WV25                     
        Pravec 2019b                   Paired with (51866) 2001 PH3.


 329291 2000 JB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 329338 2001 JW2                      
        Binzel 2019                    MITHNEOS Method: NIR


 329437 2002 OA22                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 329520 2002 SV                       
        Binzel 2019                    MITHNEOS Method: NIR


 329614 2003 KU2                      
        Binzel 2019                    MITHNEOS Method: NIR


 330825 2008 XE3                      
        Binzel 2019                    MITHNEOS Method: NIR


 331471 1984 QY1                      
        Warner 2016k                   P2 is not unique (Petr Pravec); it is not possible to
                                       attribute P1 specifically to the period of rotation and P2 to
                                       that of precession.


 331933 2004 TV14                     
        Pravec 2019b                   Paired with (63440) 2001 MD30.


 332446 2008 AF4                      
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2021h                   The results for this record are based on combining
                                       lightcurves from 2021 Jan 9-11. Additional records given the
                                       results using the data from only one of those nights.


 332685 2009 HH36                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 333358 2001 WN1                      
        Binzel 2019                    MITHNEOS Method: NIR


 334527 2002 RG189                    
        Binzel 2019                    MITHNEOS Method: sVIS


 334916 2003 YK39                     
        Pravec 2019b                   Paired with (21436) Chaoyichi.


 337066 1998 BM10                     
        Binzel 2019                    MITHNEOS Method: VIS


 337075 1998 QC1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 337181 1999 VA117                    
        Pravec 2019b                   Paired with (88259) 2001 HJ7.


 337866 2001 WL15                     
        Binzel 2019                    MITHNEOS Method: VIS


 338049 2002 NY31                     
        Binzel 2019                    MITHNEOS Method: VIS


 338176 2002 RC118                    
        Binzel 2019                    MITHNEOS Method: NIR


 339492 2005 GQ21                     
        Binzel 2019                    MITHNEOS Method: NIR


 340211 2006 AR61                     
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


 341520 Mors-Somnus                   
        Sheppard 2011                  R_orbit = 21000 ± 160 km.

        Sheppard 2012a                 Color index: g-i 1.49 ± 0.01. Delta mag between two object:
                                       0.1 mag. Orbital parameters: a = 21000 ± 160 km; e = 0.1529 M
                                       0.0028.


 341843 2008 EV5                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: VISNIR


 342842 2008 YB3                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 343098 2009 DV42                     
        Binzel 2019                    MITHNEOS Method: NIR


 344074 1997 UH9                      
        Binzel 2019                    MITHNEOS Method: VIS


 344143 2000 JQ3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 345705 2006 VB14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 345853 2007 PU11                     
        Binzel 2019                    MITHNEOS Method: NIR


 347813 2002 NP1                      
        Binzel 2019                    MITHNEOS Method: NIR


 348018 2003 SF334                    
        Pravec 2019b                   Paired with (9783) Tensho-kan.


 348400 2005 JF21                     
        Period for first entry from Oey 2016b (Date = 09/24/2015) is for the combined data set
        covering five months. Subsequent listings are for subsets within the overall span.

        Naidu 2015c                    Possible indications of a second satellite. No period for
                                       primary or orbital period of first satellite given.


 348452 2005 RU20                     
        Pravec 2019b                   Paired with (418312) 2008 FF88.


 349068 2006 YT13                     
        Binzel 2019                    MITHNEOS Method: NIR


 350513 2000 BG19                     
        Binzel 2019                    MITHNEOS Method: VIS


 350523 2000 EA14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 350716 2001 XO105                    
        Pravec 2019b                   Paired with (4765) Wasserburg.


 350751 2002 AW                       
        Pravec 2022a                   SR-SZ = 0.12 Â± 0.05


 350988 2003 GW                       
        Binzel 2019                    MITHNEOS Method: NIR


 351549 2005 TJ73                     
        Binzel 2019                    MITHNEOS Method: sVIS


 352143 2007 LR32                     
        Binzel 2019                    MITHNEOS Method: NIR


 353866 2012 WN2                      
        The designation of 2006 SU210 originally assigned to this object was updated. The MPC has
        since designated this as (353866) 2012 WN2.


 353938 1998 QR15                     
        Binzel 2019                    MITHNEOS Method: VIS


 354030 2001 RB18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 354127 2002 BP26                     
        Binzel 2019                    MITHNEOS Method: VIS


 354182 2002 DU3                      
        Binzel 2019                    MITHNEOS Method: VIS


 354652 2005 JY103                    
        Pravec 2019b                   Paired with (76111) 2000 DK106.


 354952 2006 FJ9                      
        Binzel 2019                    MITHNEOS Method: NIR


 356991 1998 QA1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 357022 1999 YG3                      
        Binzel 2019                    MITHNEOS Method: VIS


 357152 2002 CO15                     
        Binzel 2019                    MITHNEOS Method: NIR


 357439 2004 BL86                     
        Radar Team 2015a               D_primary: 0.325 km. D_satellite: 0.070 km. Discovey credit
                                       goes to Pollock et al.


 357618 2005 EM30                     
        Binzel 2019                    MITHNEOS Method: NIR


 359592 2010 VA1                      
        Binzel 2019                    MITHNEOS Method: NIR


 359995 2012 VA102                    
        The original designation was 2006 SW275. This is now identified by the MPC as 2012 VA102.

        Masiero 2009                   The original designation was 2006 SW275. This is now
                                       identified by the MPC as 2012 VA102.


 360191 1988 TA                       
        Binzel 2019                    MITHNEOS Method: NIR


 360433 2002 JR9                      
        Binzel 2019                    MITHNEOS Method: NIR


 361071 2006 AO4                      
        Binzel 2019                    MITHNEOS Method: NIR


 362310 2009 UM3                      
        Binzel 2019                    MITHNEOS Method: NIR


 363067 2000 CO101                    
        Taylor 2009                    Estimated sizes: P = 0.525 km; S = 0.045 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


 363075 2000 OG8                      
        Binzel 2019                    MITHNEOS Method: NIR


 363305 2002 NV16                     
        Binzel 2019                    MITHNEOS Method: VIS


 363505 2003 UC20                     
        Binzel 2019                    MITHNEOS Method: NIR


 363599 2004 FG11                     
        Binzel 2019                    MITHNEOS Method: TAXON


 363790 2005 JE46                     
        Binzel 2019                    MITHNEOS Method: NIR


 363814 2005 ND7                      
        Binzel 2019                    MITHNEOS Method: NIR


 364171 2006 JZ81                     
        Parker 2011                    Satellite obrital period: 4.11 ± 0.15 years.


 365071 2009 AV                       
        Binzel 2019                    MITHNEOS Method: NIR


 365246 2009 NE                       
        Binzel 2019                    MITHNEOS Method: TAXON


 365424 2010 KX7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 366774 2004 TB18                     
        Binzel 2019                    MITHNEOS Method: TAXON


 366833 2005 MC                       
        Binzel 2019                    MITHNEOS Method: NIR


 367248 2007 MK13                     
        Binzel 2019                    MITHNEOS Method: NIR


 367251 2007 PN49                     
        Binzel 2019                    MITHNEOS Method: NIR


 367922 2012 BG133                    
        Pravec 2019b                   Paired with (453106) 2007 WR62.


 367943 Duende                        
        Gary 2013a                     H, D, and pV assume a type S asteroid. A type V was also
                                       considered possible from spectrophotometric observations.

        Binzel 2019                    MITHNEOS Method: VIS

        Moskovitz 2020                 Period is post-flyby. Analysis indicates pre-flyby period of
                                       8.4 h.


 368313 2002 PY103                    
        Pravec 2019b                   Paired with (101065) 1998 RV11.


 368664 2005 JA22                     
        Binzel 2019                    MITHNEOS Method: NIR


 370037 2000 SV20                     
        Binzel 2019                    MITHNEOS Method: NIR


 370061 2000 YO29                     
        Binzel 2019                    MITHNEOS Method: VIS


 370866 2005 EB37                     
        Binzel 2019                    MITHNEOS Method: sVIS


 371660 2007 CN26                     
        Binzel 2019                    MITHNEOS Method: NIR


 374158 2004 UL                       
        Warner 2015h                   Period is a best-fit single period.


 374851 2006 VV2                      
        Binzel 2019                    MITHNEOS Method: NIR


 374855 2006 VQ13                     
        Binzel 2019                    MITHNEOS Method: NIR


 375103 2007 TD71                     
        Binzel 2019                    MITHNEOS Method: NIR


 376169 2011 BH162                    
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 376713 1995 WQ5                      
        Binzel 2019                    MITHNEOS Method: VIS


 376848 2001 RY47                     
        Binzel 2019                    MITHNEOS Method: NIR


 377732 2005 XJ8                      
        Warner 2022j                   Suspect 'wide binary'.


 380188 2000 WC67                     
        Binzel 2019                    MITHNEOS Method: VIS


 380929 2006 HU30                     
        Binzel 2019                    MITHNEOS Method: NIR


 381906 2010 CL19                     
        Binzel 2019                    MITHNEOS Method: NIR


 382758 2003 GY                       
        Binzel 2019                    MITHNEOS Method: VIS


 385186 1994 AW1                      
        Binzel 2019                    MITHNEOS Method: VIS


 385203 1999 SO15                     
        Binzel 2019                    MITHNEOS Method: TAXON


 385343 2002 LV                       
        Binzel 2019                    MITHNEOS Method: NIR


 385446 Manwe                         
        Grundy 2014                    Color indexes are for primary. The satellite showed about
                                       Ãƒâ€šÃ‚Â± 0.15 mag difference, or essentially the same color.
                                       Spin axis is for orbital pole with the primary pole presumed
                                       to be the same or very similar.

        Rabinowitz 2020                Period/amplitude are for combined system. Albedo is for
                                       primary. Orbital period for satellite is based on monomodal
                                       lightcurve.


 386298 2008 SR7                      
        Binzel 2019                    MITHNEOS Method: NIR


 388838 2008 EZ5                      
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2019web                 Suspected, low amplitude secondary period: nature
                                       undetermined.


 391151 2005 YY93                     
        Binzel 2019                    MITHNEOS Method: NIR


 393274 2013 WJ82                     
        Pravec 2019b                   Paired with (63047) 2000 WQ93.


 393359 1998 ME3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 394066 2005 XU77                     
        Binzel 2019                    MITHNEOS Method: NIR


 394130 2006 HY51                     
        Binzel 2019                    MITHNEOS Method: NIR


 396593 2001 HC                       
        Binzel 2019                    MITHNEOS Method: NIR


 398188 Agni                          
        Warner 2023a                   Final soultion required P3 = 9.48 h, A3 = 0.23 mag. P2 and P3
                                       are probably artifacts of using additive multi-period
                                       analysis on a tumbler.


 399307 1991 RJ2                      
        Binzel 2019                    MITHNEOS Method: NIR


 399418 2001 VD77                     
        Binzel 2019                    MITHNEOS Method: sVIS


 399433 2001 YK4                      
        Binzel 2019                    MITHNEOS Method: VIS


 399497 2002 TV190                    
        Masiero 2009                   Maisero et al. identified TALCS 126 as 2006 SZ2. This is a
                                       newer designation for 2002 TV190, which is the one included
                                       in the MPCORB file.


 399774 2005 NB7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 401857 2000 PG3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 402267 2005 QE166                    
        Binzel 2019                    MITHNEOS Method: NIR


 403049 2008 AY36                     
        Binzel 2019                    MITHNEOS Method: NIR


 405058 2001 TX16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 407656 2011 SL102                    
        Binzel 2019                    MITHNEOS Method: NIR


 408792 2000 GF2                      
        Binzel 2019                    MITHNEOS Method: NIR


 409156 2003 UW156                    
        Pravec 2019b                   Paired with (226268) 2003 AN55.


 409204 2003 WX25                     
        Binzel 2019                    MITHNEOS Method: NIR


 409995 2006 WV3                      
        Binzel 2019                    MITHNEOS Method: NIR


 410195 2007 RT147                    
        Binzel 2019                    MITHNEOS Method: NIR


 410627 2008 RG1                      
        Binzel 2019                    MITHNEOS Method: NIR


 410650 2008 SQ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 410778 2009 FG19                     
        Binzel 2019                    MITHNEOS Method: NIR


 411280 2010 SL13                     
        Binzel 2019                    MITHNEOS Method: NIR


 412065 2013 ET86                     
        Pravec 2019b                   Paired with (11677) 1998 DY4.


 412976 1987 WC                       
        Binzel 2019                    MITHNEOS Method: NIR


 413038 2001 MF1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 413123 2001 XS1                      
        Binzel 2019                    MITHNEOS Method: VIS


 413563 2005 TG45                     
        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       90.5-64.4 deg. The H_SR values are the linear extrapolation
                                       using the phase slope (beta_SR) of 0.03259. The lack of low
                                       phase angles prevented use of H-G or HG1,G2 modeling.


 413577 2005 UL5                      
        Pravec 2015web                 Secondary period might be due to being binary.

        Binzel 2019                    MITHNEOS Method: NIR


 414166 2008 AU67                     
        Pravec 2019b                   Paired with (56700) 2000 LL28.


 414287 2008 OB9                      
        Binzel 2019                    MITHNEOS Method: NIR


 414586 2009 UV18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 414990 2011 EM51                     
        Binzel 2019                    MITHNEOS Method: NIR


 415711 1998 WT7                      
        Binzel 2019                    MITHNEOS Method: NIR


 415949 2001 XY10                     
        Binzel 2019                    MITHNEOS Method: VIS


 415992 2002 AT49                     
        Pravec 2019b                   Paired with (87887) 2000 SS286.


 416151 2002 RQ25                     
        Binzel 2019                    MITHNEOS Method: NIR


 416186 2002 TD60                     
        Warner 2015r                   Period analysis by Pravec (Czech Institute).

        Binzel 2019                    MITHNEOS Method: VISNIR


 416195 2002 TR190                    
        Binzel 2019                    MITHNEOS Method: NIR


 416231 2003 AJ73                     
        Binzel 2019                    MITHNEOS Method: NIR


 416591 2004 LC2                      
        Binzel 2019                    MITHNEOS Method: TAXON


 416680 2004 XD50                     
        Binzel 2019                    MITHNEOS Method: TAXON


 416694 2004 YR32                     
        Warner 2021g                   Suspected very wide binary, which would make the 50-h period
                                       that of the primary's rotatation, not the orbital period of
                                       the satellite.


 418312 2008 FF88                     
        Pravec 2019b                   Paired with (348452) 2005 RU20.


 418797 2008 VF                       
        Binzel 2019                    MITHNEOS Method: NIR


 419464 2010 CC180                    
        Binzel 2019                    MITHNEOS Method: NIR


 420187 2011 GA55                     
        Binzel 2019                    MITHNEOS Method: NIR


 420738 2012 TS                       
        Binzel 2019                    MITHNEOS Method: NIR


 421781 2014 QG22                     
        Pravec 2019b                   Paired with (53576) 2000 CS47.


 422686 2000 AC6                      
        Binzel 2019                    MITHNEOS Method: VIS


 423321 2005 ED318                    
        Binzel 2019                    MITHNEOS Method: NIR


 428086 2006 NM                       
        Binzel 2019                    MITHNEOS Method: NIR


 430439 2000 LF6                      
        Binzel 2019                    MITHNEOS Method: TAXON


 430484 2001 ST246                    
        Chang (2015) H values are based on H-G system. The G values are in R, not V. All lightcurves
        with a period were given U = 2 regardless of rating by Chang et al.


 430804 2005 AD13                     
        Binzel 2019                    MITHNEOS Method: NIR


 433939 1995 DW1                      
        Binzel 2019                    MITHNEOS Method: NIR


 433953 1997 XR2                      
        Pravec 2019web                 Second period in tumbling solution is not unique.


 434096 2002 GO5                      
        Binzel 2019                    MITHNEOS Method: NIR


 436459 2011 CL97                     
        Pravec 2019b                   Paired with (49791) 1999 XF31.


 436551 2011 GD83                     
        Pravec 2019b                   Paired with (16815) 1997 UA9.


 437841 1998 HD14                     
        Binzel 2019                    MITHNEOS Method: TAXON


 437844 1999 MN                       
        Binzel 2019                    MITHNEOS Method: TAXON


 437905 2001 XU30                     
        Binzel 2019                    MITHNEOS Method: VIS


 438105 2005 GO22                     
        Binzel 2019                    MITHNEOS Method: NIR


 440212 2004 OB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 441549 2008 TM68                     
        Pravec 2019b                   Paired with (43008) 1999 UD31.


 442523 2011 WU95                     
        Binzel 2019                    MITHNEOS Method: NIR


 443103 2013 WT67                     
        Warner 2015c                   Period is estimate for one of the two tumbling periods.


 443837 2000 TJ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 445775 2011 YA                       
        Binzel 2019                    MITHNEOS Method: NIR


 446085 2013 CW179                    
        Pravec 2019b                   Paired with (66659) 1999 TJ1.


 446791 1998 SJ70                     
        Binzel 2019                    MITHNEOS Method: NIR


 446804 1999 VN6                      
        Binzel 2019                    MITHNEOS Method: VIS


 448003 2008 DE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 448972 2011 YV15                     
        Binzel 2019                    MITHNEOS Method: NIR


 450293 2004 LV3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 450894 2008 BT18                     
        Benner 2008a                   Arecibo and Goldstone observations show: D1: 0.6 km D2: >0.2
                                       km Sep: 1.5 km.

        Warner 2018h                   No sign of primary rotatin of about 2.5 h.

        Binzel 2019                    MITHNEOS Method: NIR


 451124 2009 KC3                      
        Binzel 2019                    MITHNEOS Method: NIR


 451157 2009 SQ104                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 451397 2011 EZ78                     
        Pravec 2011web                 Two suspect attentuations were seen but not confirmed.

        Skiff 2011web                  Data suggests possibility of tumbling or binary.

        Binzel 2019                    MITHNEOS Method: VISNIR


 452334 2001 LB                       
        Binzel 2019                    MITHNEOS Method: NIR


 452389 2002 NW16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 452561 2005 AB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 452773 2006 DM14                     
        Binzel 2019                    MITHNEOS Method: sVIS


 452807 2006 KV89                     
        Binzel 2019                    MITHNEOS Method: NIR


 453106 2007 WR62                     
        Pravec 2019b                   Paired with (367922) 2012 BG133.


 453563 2010 BB                       
        Binzel 2019                    MITHNEOS Method: NIR


 453818 2011 SJ109                    
        Pravec 2019b                   Paired with (25021) Nischaykumar.


 455157 1997 YM3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 455185 2000 EB107                    
        Binzel 2019                    MITHNEOS Method: TAXON


 455192 2000 QN130                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 455213 2001 OE84                     
        Binzel 2019                    MITHNEOS Method: VIS


 455322 2002 NX18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 455327 2002 OP28                     
        Pravec 2019b                   Paired with (9068) 1993 OD.


 455415 2003 GA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 455426 2003 MT9                      
        Binzel 2019                    MITHNEOS Method: NIR


 455578 2004 RA216                    
        Binzel 2019                    MITHNEOS Method: sVIS


 455594 2004 SV55                     
        Binzel 2019                    MITHNEOS Method: TAXON


 456301 2006 SV134                    
        Binzel 2019                    MITHNEOS Method: NIR


 459200 2012 DK61                     
        Binzel 2019                    MITHNEOS Method: NIR


 461501 2003 FT3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 461852 2006 GY2                      
        Benner 2006b                   Secondary diameter estimated to be 0.08 km and orbital
                                       separation at least 0.5 km.


 461912 2006 RG2                      
        Binzel 2019                    MITHNEOS Method: NIR


 462176 2007 TC334                    
        Pravec 2019b                   Paired with (70511) 1999 TL103.


 464797 2004 FZ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 464798 2004 JX20                     
        Skiff 2019web                  The solutions are not unique.


 464815 2004 RV257                    
        Binzel 2019                    MITHNEOS Method: sVIS


 465402 2008 HW1                      
        Binzel 2019                    MITHNEOS Method: NIR


 465616 2009 EC                       
        Warner 2016m                   Suspected very wide binary.


 467317 2000 QW7                      
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2020c                   Two possibilities: single period with large zero-point
                                       offsets or tumbling with near zero offsets.


 467336 2002 LT38                     
        Warner 2023f                   P1 is dominant, though it may still be a multiple of the true
                                       frequency (1/P1). P2 is one of several solutions but it is
                                       the one that gave the best fit when subtracting from the raw
                                       data.


 467460 2006 JF42                     
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2022web                 Alternate solutions ampltides assumed to be the same as the
                                       adopted period.


 468738 2010 TN54                     
        Binzel 2019                    MITHNEOS Method: NIR


 469438 2002 GV31                     
        Pal 2015b                      V-R assumed.


 469446 2002 NL8                      
        Binzel 2019                    MITHNEOS Method: sVIS


 469513 2003 QR79                     
        Binzel 2019                    MITHNEOS Method: VIS


 469896 2005 WC1                      
        Miles 2008b                    Given period based on 3 nights (Miles, private
                                       communications). JBAA publication gives period of 2.57 h base
                                       on one night.


 470004 2006 MJ10                     
        Binzel 2019                    MITHNEOS Method: NIR


 470975 2009 SC15                     
        Binzel 2019                    MITHNEOS Method: VIS


 471240 2011 BT15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 474158 1999 FA                       
        Binzel 2019                    MITHNEOS Method: VIS


 474370 2002 RT157                    
        Binzel 2019                    MITHNEOS Method: sVIS


 475665 2006 VY13                     
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2022j                   Secondary period is almost 3:1 with dominant period and may
                                       be a harmonic artifcat of the analysis.


 477465 2009 XZ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 477762 2010 XZ67                     
        Binzel 2019                    MITHNEOS Method: NIR


 479358 2013 XN8                      
        Pravec 2019b                   Asteroid pair with 5478 Wartburg.


 480820 1998 VF32                     
        Binzel 2019                    MITHNEOS Method: NIR


 480858 2001 PT9                      
        Binzel 2019                    MITHNEOS Method: NIR


 480883 2001 YE4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 481032 2004 YZ23                     
        Binzel 2019                    MITHNEOS Method: NIR


 481085 2005 SA135                    
        Pravec 2019b                   Paired with (21028) 1989 TO.


 481090 2005 SY173                    
        Binzel 2019                    MITHNEOS Method: sVIS


 481532 2007 LE                       
        Brozovic 2012                  Estimated sizes: Dp 0.5 km; Ds 0.18 km. Orbital separation >
                                       0.8 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


 481542 2007 RF5                      
        Binzel 2019                    MITHNEOS Method: NIR


 482250 2011 LL2                      
        Pravec 2022web                 Seconary solution amplitude assumed to be the same as the
                                       primary amplitude.


 482796 2013 QJ10                     
        Binzel 2019                    MITHNEOS Method: NIR


 483422 2000 CE59                     
        Binzel 2019                    MITHNEOS Method: VIS


 483423 2000 DO1                      
        Binzel 2019                    MITHNEOS Method: VIS


 484757 2009 BL2                      
        Binzel 2019                    MITHNEOS Method: NIR


 484976 2009 UN3                      
        Binzel 2019                    MITHNEOS Method: NIR


 485051 2010 CM44                     
        Binzel 2019                    MITHNEOS Method: NIR


 486958 Arrokoth                      
        Porter 2019                    Diamter is volume of equivalent sphere based on the overall
                                       dimensions of the contact binary system. The individual
                                       volumes are 15.9 km and 12.9 km.

        Stern 2019                     Effective diameter (from volume): Ultima: 13.88 km; Thule:
                                       12.61 km. Phase angle is viewed from Earth.

        Hofgartner 2021                Viewing aspect is from Earth.


 488453 1994 XD                       
        Binzel 2019                    MITHNEOS Method: NIR


 488515 2001 FE90                     
        Binzel 2019                    MITHNEOS Method: TAXON


 489337 2006 UM                       
        Binzel 2019                    MITHNEOS Method: NIR


 492143 2013 OE                       
        Warner 2020c                   A third period was found as well: P3 = 4.88 h.


 495833 2000 SB8                      
        Binzel 2019                    MITHNEOS Method: NIR


 495858 2003 MJ4                      
        Binzel 2019                    MITHNEOS Method: NIR


 496001 2007 VR183                    
        Binzel 2019                    MITHNEOS Method: NIR


 496028 2008 SC9                      
        Pravec 2019b                   Paired with (14806) 1091 EV25.


 496923 2001 UW57                     
        Originally Derm3d in Dermawan Ph.D. thesis.


 497676 2006 SR2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 500080 2011 WV134                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 501710 2014 UY23                     
        Pravec 2019b                   Paired with (88666) 2001 RP79.


 503861 1998 WZ1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 503871 2000 SL                       
        Binzel 2019                    MITHNEOS Method: sVISNIR


 503941 2003 UV11                     
        Binzel 2019                    MITHNEOS Method: NIR


 503955 2004 ED107                    
        Pravec 2019b                   Paired with (53537) 2000 AZ239.


 504025 2005 RQ6                      
        Binzel 2019                    MITHNEOS Method: NIR


 504887 2010 WL                       
        Binzel 2019                    MITHNEOS Method: NIR


 505476 2013 UL15                     
        Alexandersen 2018              Applies to all Alexandersen 2018: For those objects in their
                                       list that were found in MPCOrb, the Hv magnitude was nearly
                                       the same as their Hr (Pan-STARRS r). The original Hr is
                                       reported in the detail record _and_ used for H in the summary
                                       table if an MPCOrb value was not available.


 506437 2000 WL10                     
        Binzel 2019                    MITHNEOS Method: VIS


 506459 2002 AL14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 508774 1999 JE1                      
        Binzel 2019                    MITHNEOS Method: VIS


 508908 2003 YX1                      
        Binzel 2019                    MITHNEOS Method: VIS


 510132 2010 UY57                     
        Pravec 2019b                   Paired with (6369) 1983 UC.


 514596 2003 FG                       
        Binzel 2019                    MITHNEOS Method: NIR


 516398 2001 HW15                     
        Binzel 2019                    MITHNEOS Method: VIS


 516420 2003 FS2                      
        Binzel 2019                    MITHNEOS Method: VIS


 516435 2004 FJ29                     
        Binzel 2019                    MITHNEOS Method: NIR


 518482 2005 TZ42                     
        Binzel 2019                    MITHNEOS Method: sVIS


 518507 2006 EE1                      
        Binzel 2019                    MITHNEOS Method: NIR


 518810 2010 CF19                     
        Binzel 2019                    MITHNEOS Method: NIR


 523625 2008 DG17                     
        Warner 2018h                   2018 radar observations indicate a period of ~2.8 h, but a
                                       slightly longer period is possible. The photometric data do
                                       not allow formally excluding a solution near 7.3 h.


 523775 2014 YB35                     
        Naidu 2015b                    Ds: < 150 m.


 523806 2002 WW17                     
        Cutri 2019                     The analysis used W1 and W2 NEOWISE data.

        Cutri 2019                     The analysis used W1 and W2 NEOWISE data.


 523855 1995 SK87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 523856 1995 SL87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 525939 2005 UY97                     
        Pravec 2019b                   Paired with (229401) 2005 SU152.


 528159 2008 HS3                      
        Warner 2019p                   Single period analysis found several dominant periods. They
                                       are listed in the Ambiguous table.


 528407 2008 TO52                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 531119 2012 FF11                     
        Pravec 2019b                   Paired with (69298) 1992 DR9.


 531260 2012 KL9                      
        Pravec 2019b                   Paired with (313701) 2003 UN3.


 532037 2013 FY27                     
        Sheppard 2018c                 Separation from primary about 9800 km.


 537342 2015 KN120                    
        Warner 2018a                   P3/A3: 7.448 ± 0.006, 0.12 ± 0.03 mag. P2 and P3 may be a
                                       single period corrupted by harmonics of P1, or P1 and the
                                       true P2 are tumble frequencies beating to produce a third
                                       apparent frequency.


 541818 2012 AX10                     
        Pravec 2019b                   Paired with (33325) 1998 RH3.


 545135 2014 YE64                     
        Binzel 2019                    MITHNEOS Method: sVIS


 554099 2012 KU50                     
        Chandler 2021                  Binary discovery. Semi-major axis > 15000 km.


 561272 2015 RV228                    
        Pravec 2019b                   Paired with (98866) Giannabussolari.


 575395 2011 SE164                    
        Pravec 2019b                   Paired with (100440) 1996 PJ6.


 576293 2012 LB9                      
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 577283 2013 CT63                     
        Pravec 2019b                   Paired with (63970) 2001 SG72.


 590180 2011 SR158                    
        Pravec 2019b                   Paired with (8306) Shoko.


 606952 2019 WF6                      
        The period is an approximaation of a short-term periood superimpoed on a longer period, or
        the dominant period of a tumbler.


 611007 2006 QN54                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.


 612023 1994 VX3                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 612050 1997 GL3                      
        Skiff 2023                     The given period is for an apparent short-term component of
                                       the overall lightcurve. This may be an artifact or an element
                                       of a tumbler.


 612147 2000 CF105                    
        Parker 2011                    Satellite orbital period: 10.92 ± 0.12 years.


 612242 2001 QQ322                    
        Noll 2008d                     No lightcurve observations per se. Two components of about
                                       equal size separated by 0'.1272 ± 0'.0015, or about 4000 km.
                                       


 612687 2003 UN284                    
        Parker 2011                    Satellite orbital period: 8.73 ± 0.65 years.


 612813 2004 RF84                     
        Benner (2006a) observed with radar and found a dimension of at least 1.2 km based on echo
        delay range. However, the images indicate the possibility of a bifurcated body with an
        effective diameter of about 1.5 km. Based on the total information, we presumed a dark
        (C-type) asteroid and used the default albedo for that class and MPCORB H to derive a
        diameter.


 612929 2005 CR37                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


 613512 2006 SK134                    
        Warner 2019m                   The two periods given for this likely tumbler are best-fit
                                       single periods and not formal two-period analysis.


 614473 2009 SZ67                     
        Pravec 2019b                   Paired with (105247) 2000 QH3.


 616600 2006 AN29                     
        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 620071 2011 WN15                     
        Pravec 2019web                 Possible color variations during rotation.


      0 103P/Hartley                  
        Harmon 2010                    The diameter is based the long-axis dimension of a
                                       highly-elongated, bilobate object as observed by radar. The
                                       radar cross section was 0.04 km^2, which corresponds to a
                                       diameter of ~100 m.


      0 10P/Tempel 2                  
        A'Hearn 1989                   Amplitude is for observations at 4845 Angstroms. Other
                                       amplitudes: 6840 A, 0.45 mag; 10100 A, 0.8 mag.


      0 169P/NEAT                     
        Determined to be a comet (by Warner) after receiving an asteroid designation. Current MPC
        designation is P/2002 EX12.


      0 1994 CJ1                      
        Radar Team 2014b               First estimate is two 100-m bodies about 500-m apart.


      0 1994 ES2                      
        Terai 2018                     Entries for Terai 2017 in the Color Index table were derived
                                       from their Hg-r and Hr-i. The errors were found by adding the
                                       individual errors in quadrature.


      0 1998 WV24                     
        Benecchi 2008                  The two components were separated by an angular distance of
                                       0'.051 ± 0'.002, with the secondary fainter by 0.3 magnitude.
                                       The secondary was located at 0'.033 ± 0'.003 in R.A. and
                                       0'.039 ± 0'.003 in Decl. relative to the primary.


      0 1999 TE21                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


      0 2000 UK11                     
        Nolan 2001                     It appears that Nolan made a factor of 2 error in his
                                       reported period. The LCDB adopts the 0.025 h period based on
                                       the reported observational data of radar bandwidth and
                                       estimated size of 30 meters.


      0 2001 QW322                    
        Parker 2011                    Satellite orbital period: 17.01 ± 1.55 years.


      0 2001 RW17                     
        Warner 2020a                   8-hour solution unlikely but cannot be formally excluded.


      0 2003 QY90                     
        Benecchi 2009                  See note under 2001 QC298.

        Grundy 2011                    Orbital period determined from astrometric measurements.


      0 2005 GQ107                    
        Pravec 2019b                   Paired with (55913) 1998 FL12.


      0 2005 LW3                      
        Naidu 2022                     Primary-Seoncdary distance ~ 4 km.


      0 2005 WW113                    
        Pravec 2019b                   Paired with (5026) Martes.


      0 2006 BR284                    
        Parker 2011                    Satellite orbital period: 4.11 ± 0.04 years.


      0 2006 CH69                     
        Parker 2011                    Satellite orbital period: 3.89 ± 0.07 years.


      0 2006 SF369                    
        Noll 2008b                     No lightcurves per se. Hubble observations show a binary
                                       system of about the same size separated by 0'.109 ± 0'.003,
                                       or about 3200 km.


      0 2007 TQ24                     
        Warner 2020c                   Second period is ambiguous. Alternate solution: P_2B: 9.57 h.


      0 2008 SD                       
        The geocentric phase angle and PAB in the Masiero 2020b details records were computed using
        the mean MJD given in the file. H-G are the values used for the model and appear only in
        details records. The MPCORB H-G at the time of import are used in the summary line. The
        albedo error is the larger linear error listed in the table. The diameter is the corrected
        value (see Masiero et al. 2020b).

        Masiero 2020b                  The geocentric phase angle and PAB in the Masiero 2020b
                                       details records were computed using the mean MJD given in the
                                       file. H-G are the values used for the model and appear only
                                       in details records. The MPCORB H-G at the time of import are
                                       used in the summary line. The albedo error is the larger
                                       linear error listed in the table. The diameter is the
                                       corrected value (see Masiero et al. 2020b).


      0 2008 TC3                      
        Aleshkina 2011                 Periods of 18 m and 6.89 h were also reported. The LCDB
                                       authors believe these to be spurious, possibly because
                                       non-principal axis rotation was not taken into account.


      0 2008 TT26                     
        Ryan 2009                      http://infohost.nmt.edu/~bryan/research/work/mro_images/k08t2
                                       6t/k08t26t_081019.jpg


      0 2008 UZ220                    
        Pravec 2019b                   Paired with (103055) 1999 XR134.


      0 2009 BD                       
        Mommert 2014c                  Diameter and albedo based on a rocky body. An equally likely
                                       solution assuming a collection of bare rock slabs gives D =
                                       0.004 ± 0.001 km and pV = 0.45 ± 0.35.


      0 2009 QZ66                     
        This note applies to all Lo et al. (2020, AJ 159) entries. A suffix of 'Lo21-' has been
        added to the all-numeric internal IDs used by Lo et al. to avoid confusion with an
        MPC-assigned number. The astrometric data they provided was used to match each of their
        objects to one in the MPCOrb data set. In most cases, the cross-match was unambiguous. For
        the others, there will be an entry in the extended notes for that particular Lo et al.
        details record. This is particularly important for objects in the summary line that have
        only the Lo et al. reference and are flagged as uncertain. Here, the object listed may not
        be the correct one. The Date, PAB_L, PAB_B, and Phase entries in the details record are
        based on 1) the cross-matched ID and 2) the first date of observations, which usually
        spanned about three days.


      0 2010 RC130                    
        Skiff 2019b                    Analysis by P. Pravec. A single period of 8.687 h was
                                       initially found, but this is a beat period based on a 3:5
                                       ratio of the periods found with 2-dimensional Fourier
                                       analysis. The periods could be a linear combination of the
                                       two actual periods (precession and rotation).


      0 2010 WC9                      
        Beniyama 2022                  This applies to all Beniyama 2022 entries: the observations
                                       were made with a video camera taking multiple frams per
                                       second.


      0 2011 CT4                      
        Pravec 2020web                 A higher than normal albedo was used to calculate a revised
                                       diameter based on the new H-G values.


      0 2011 FJ54                     
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2011 HP                       
        Warner 2019p                   Period and amplitudes based on full data set.


      0 2011 TG2                      
        Warner 2023a                   Period of combined data set.


      0 2011 UT239                    
        Masiero 2009                   At the time of the TALCS survey, this object had the
                                       desgination of 2006 SP242. The MPCORB file not identifies it
                                       as 2011 UT239.


      0 2011 XA3                      
        Urakawa 2014                   H, D, and pV assume a type S asteroid. A type V was also
                                       considered possible from spectrophotometric observations.


      0 2012 LZ1                      
        Hicks 2012d                    Authors gave period as 5-16 hours. The two periods given are
                                       the approximae values based on their period spectrum from
                                       Fourier analysis.

        Howell 2012b                   The diameter is the approximate effecitve diameter based on a
                                       longest dimension of about 1 km. The albedo is the average of
                                       the range estimated based on H = 19.8.


      0 2012 PG6                      
        Warner 2023a                   Result of 2022 Sep 24+28.

        Warner 2023a                   Result of combined data set.

        Warner 2023a                   Result of 2022 Sep 26+28.

        Warner 2023a                   Result of 2022 Sep 24+26.


      0 2012 TC4                      
        Urakawa 2019                   Period is for precession. NPAR P2 is rotation period.


      0 2012 TK84                     
        Pravec 2019b                   Paired with (167405) 2003 WP118.


      0 2012 TS209                    
        Pravec 2019b                   Paired with (26420) 1999 XL103.


      0 2012 UX136                    
        Pravec 2012web                 Based on data from Joe Pollock.


      0 2014 AC                       
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2014 AN51                     
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2014 CH9                      
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2014 EX61                     
        2016 UV197 may have been the designation at the time. Using the MPC MP Checker, the
        astrometric position from Lo et al. (2020), 2014 EX61 has the exact same position. Since
        2016 UV197 is no longer an recognized designation, 2014 EX61 was assumed to be the actual
        object.

        Lo 2020                        2016 UV197 may have been the designation at the time. Using
                                       the MPC MP Checker, the astrometric position from Lo et al.
                                       (2020), 2014 EX61 has the exact same position. Since 2016
                                       UV197 is no longer an recognized designation, 2014 EX61 was
                                       assumed to be the actual object.


      0 2014 ET121                    
        Lo 2020                        The designation at the time was likely 2016 UG159, which
                                       appears and shows the same position as 2014 ET121 in the MPC
                                       MPChecker. However, 2016 UG159 is no longer an assigned
                                       designation and so 2014 ET121 was used for this object.


      0 2014 GN1                      
        Hicks 2014d                    V-R = 0.40 assumed to give H = 24.1


      0 2014 JO25                     
        Aznar 2019b                    The primary record for Aznar 2019b gives the best-fit for the
                                       entire data set. The subsequent entires are based on subsets
                                       obtained by different observers throughout the runs of 2017
                                       April 20 to May 17.

        Venkataramani 2019             The actual phange angle ranged from 61 to 50 degrees over the
                                       course of the observations. During that time, the B-V color
                                       index increased (bluer) from 0.61 to 0.98 while the V-R index
                                       remained nearly constant.


      0 2014 MK6                      
        Navarro-Meza 2019              This note applies to all Navarro-Meza 2019 color index
                                       entries. The paper gave r-i colors after substracting solar
                                       color but that value was not given. A value of r-i(sun) =
                                       0.11(*) mag was added to the values in the paper for the
                                       listings in the color index tabel.
                                       http://classic.sdss.org/dr5/algorithms/sdssUBVRITransform.htm
                                       l


      0 2014 SC324                    
        Warner 2015h                   P2 in NPAR table is not unique. Low amplitude tumbler:
                                       A2/A1_secondharmonic ~ 0.21.


      0 2014 VR4                      
        Pravec 2019b                   Paired with (46829) McMahon.


      0 2014 WK368                    
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2015 AH1                      
        Pravec 2019b                   Paired with (16126) 1999 XQ86.


      0 2015 OH                       
        Warner 2016c                   Ambiguous: P_alt: 2.630 cannot be formally excluded but is
                                       not likely.


      0 2015 OS35                     
        Ieva 2018                      Computed phase angle significantly different from that in
                                       paper. Possible wrong date or object.


      0 2015 RF36                     
        Taylor 2015b                   Period estimated from spread of CW radar data


      0 2016 AZ8                      
        Virkki 2019                    The periods are based on upper limits and accounting for the
                                       mutual orbit plane being inclined several tens of degrees
                                       from the line of sight.

        Warner 2019m                   The orbital period is based on the lightcurve having the
                                       expected mutual events. The primary period seems much too
                                       long compared to initial radar observations.


      0 2016 BU13                     
        Warner 2016m                   Suspected P3 = 16.46 ± 0.02, A3 = 0.04 ± 0.01


      0 2016 CA138                    
        Borisov 2023                   Sidereal periods (h):  Pole 1: 5.3137 Pole 2: 5.3141 Pole 3:
                                       5.3139 Pole 3 mirror: 5.3139


      0 2016 EV27                     
        Warner 2016j                   Second period may be artificat of Fourier analysis. However,
                                       the two periods do not have a simple integral multiple ratio.
                                       


      0 2016 UW187                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2016 UZ215                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2016 UC230                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2017 BW                       
        Pravec 2017web                 Second period is no unique. First period could be rotation or
                                       precession.


      0 2017 NH                       
        Warner 2018a                   Second NPA period is one of many possibilities.


      0 2017 SL16                     
        Borisov 2023                   Sideral period for each pole: (190.4,34.3,0.3188)
                                       (183.7,-75.8,0.3190) (233.6,53.6,0.3192) (97.2,-41.2,0.3191)
                                       


      0 2017 YH                       
        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       87.1-90.3 deg.


      0 2017 YE5                      
        JPL 2018                       Each body about 900 m, widely separated (~2500 m).


      0 2018 AJ                       
        Warner 2018k                   Second period may be actual second period or linear
                                       combination of the two frequencies of NPA rotation with the
                                       main frequency.


      0 2018 CB                       
        Birtwhistle 2021a              The phase angle for the breakout entries was forced to the
                                       mid-phase angle of the observations. The phase angle bisector
                                       values are for 00:00h UT on 2018 Feb 9.


      0 2018 JE1                      
        Warner 2018m                   Secondary period is likely wrong, even spurious. It was
                                       needed to overcome an excessively large nightly zero point
                                       shift of 0.8 mag.


      0 2018 KE3                      
        Warner 2019b                   Possible very wide binary, in which case the primary period
                                       is the longer of the two. The shorter period is rated U=3;
                                       the secondary period is U=2.


      0 2018 LK                       
        Warner 2018m                   Period is for combined data set from 2018 June 12-13.
                                       Individual results are reported seperatedly.


      0 2018 TF3                      
        Pravec 2018b                   The secondary period/amplitude given in the LC_BINARY table
                                       are for the synchronous satellite.

        Warner 2019f                   Orbital period derived from half-period analysis that allowed
                                       full coverage of the P_orb lightcurve.


      0 2018 UQ1                      
        Lopez-Oquendo 2019a            Longer solution of 7.1 h is likely a double-period fit by
                                       exclusion.


      0 2018 UD3                      
        Beniyama 2022                  Given the amplitude and assuming the original period is
                                       correct, the true period may be ~0.0165112 h.


      0 2018 XV5                      
        Pravec 2022web                 Amplitude for P2 (A2) not given so listed as the same as P1.

        Warner 2022i                   Periods 2 and 3 are artifacts of additive period analysis,
                                       which does not properly handle tumbling asteroids.


      0 2019 FP2                      
        Warner 2019p                   Extrmely noisy data with no discernible trends.


      0 2019 KZ3                      
        Warner 2019p                   A nearly as-good single period solution could also be found.
                                       The RMS scatter was higher by about 0.04 mag.


      0 2019 SH6                      
        Warner 2020c                   Two periods given were derived from subtracting an 8.22 h,
                                       0.19 mag lightcurve. This may be a 'beat frquency' period.


      0 2019 UC                       
        A super-short period (Pravec et al., 2019) is a possibility.


      0 2020 AZ2                      
        Pravec 2020b                   Satellite A = 0.07 mag, a/b = 1.23.


      0 2020 BX12                     
        Virkki 2020                    Diameter of 180 m is for projected-area-equivalent.
                                       Primary/Second sizes: 165 m and 70 m. An orbital period of
                                       15-16 not ruled out.


      0 2020 HS7                      
        Beniyama 2022                  Two observations on same date: midtimes: 14:36:31 amd
                                       16:24:21.


      0 2020 KK7                      
        Birtwhistle 2021a              H-G were determined using the lightcurve peak instead of
                                       average.


      0 2020 ST1                      
        Warner 2021d                   Pravec found the strongest solutions to be 1.879, 2.879, and
                                       5.407 h. Two are real, the third is related to the other two.
                                       Note that 1/2.879 = 1/1.879 - 1/5.407.


      0 2020 TP1                      
        Birtwhistle 2021e              The stated period and secondary in the NPAR table are not
                                       secure but simply two dominant periods found using software
                                       that properly handles tumbling asteroids.


      0 2021 DW1                      
        Kwiatkowski 2021               SG-SI: 0.79 Â± 0.01. The phase angle values are for 0h UT on
                                       the given date. They can be significantly different from the
                                       value at the actual time of observations.


      0 2021 DX1                      
        Warner 2021h                   The second period in the NPA table is one of several
                                       possibilities.


      0 2021 KN2                      
        Birtwhistle 2021c              P3: 0.012516(2) h, A3: 0.27.  1/P1 = 2/P3 - 2/P2


      0 2022 DA                       
        Period/amplitude could not be determined.

        Birtwhistle 2022b              Period/amplitude could not be determined.


      0 2022 LV                       
        Pravec 2022web                 Amplitude for P2 (A2) assumed to be the same as A1.


      0 2022 NE                       
        Birtwhistle 2023a              P3 = 0.01217 Â± 0.00001 h; A3 = 0.4 Â± 0.4 mag.


      0 2022 QT7                      
        Birtwhistle 2023a              P3 = 0.0147778 Â± 0.0000015 h; A3 = 0.7 Â± 0.5 mag.


      0 2023 HK                       
        Birtwhistle 2023d              The phase angle ranged from 50.5 to 72.3 over the span of the
                                       observations. The full range of the tumbling amplitude is
                                       ~1.5 mag.


      0 2023 HU4                      
        Birtwhistle 2023d              The second period is ambiguous. An alternate solution is P2 =
                                       0.1714 (0.0003) h, A = 0.4 (0.2) mag. The phase angle ranged
                                       from 15.0-11.8 deg over the span of the observations. The
                                       full range of the tumbling amplitude is ~1.3 mag.


      0 2023 HO18                     
        Birtwhistle 2023d              The phase angle ranged from 41.8 to 17.1 deg over the span of
                                       the observations. Using default G = 0.15 led to an offset of
                                       0.44 mag between two night and significant deviation from the
                                       predicted magnitudes using G = 0.15..


      0 2023 KZ1                      
        Birtwhistle 2023d              Indications of a long secondary period. Based on the raw
                                       plot, a solution might be P2 ~ 0.24 h for a bimodal curve
                                       [LCDB authors].


      0 C/2003 WT42                   
        Determined to be a comet after discovery and given asteroid designation. Current MPC
        designation is C/2003 WT42.


      0 Derm0a                        
        Dermawan 2002b, Doctoral Thesis This paper included approximately 50 objects, named in this
        list as DermXx, with X being a number and x a letter. The paper used the following values,
        which were adopted in lieu of the defaults used in this publication that are based on the
        semi-major axis:  SMA: 2.3 < a < 2.8, Type = C, V-R = 0.53±0.04, Pv = 0.21±0.05;   SMA: 2.8
        < a < 3.3, Type = C, V-R = 0.37±0.03, Pv = 0.06±0.02.  The listed diameters are those listed
        by Dermawan as computed from these assumed values and his measured value of Hv.


      0 Derm1c                        
        Dermawan 2011                  Only 22 data points.


      0 Derm2b                        
        Dermawan 2011                  D flag applies to amplitude only.


      0 Derm2h                        
        Dermawan 2011                  D flag applies to amplitude only.


      0 Derm2K                        
        Dermawan 2011                  Only 18 data points.


      0 Derm2O                        
        Dermawan 2011                  Only 9 data points.


      0 Derm3b                        
        Dermawan 2011                  Any number of period solutions are possible.


      0 Derm4m                        
        Dermawan 2011                  Dermawan paper gave amplitude as A = 0.35. It should have
                                       been 0.035. The value was rounded up to 0.04 mag for entry.


      0 Derm6e                        
        Dermawan 2011                  R = 24.


      0 Derm6j                        
        Dermawan 2011                  R = 24.


      0 FOSL01010327                  
        Chang 2022b                    This applies to all Chang 2022b; Ap. J. Suppl. Ser. 259,
                                       id.7. The filter band was r2 for all observations other than
                                       Apr 10, 2019, which used the SG filter. 'r2' is not
                                       recognized in the LCDB, so SR (Sloan r') is given. The
                                       reported diameters do not always agree with the standard
                                       formula using H and albedo to find a diameter. The summary
                                       line uses the value of the standard formula.


      0 FSAP04010083                  
        This note applies to all Chang 2021 (PSJ 2) entries. The observations were made in g and r2
        bands. The photometric bands (for H) were assigned as SG and SR, respectively. The H_SR
        values were transformed to approximate V by using the LCDB V = SR+ 0.22. While not exact,
        this makes the values more compatible to H_V when plotting frequency-diameters. For diameter
        calculations, an albedo of 0.05 and G = 0.15 Ã‚Â± 0.2 was assumed for both bands. Only some
        of the 53 objects could be tied to an object in the MPC database. For those without ID, and
        where possible, the phase and phase angle bisector values were assumed to be the same as for
        an identified object in the same observing block. The entries are flagged as being from a
        Sparse Wide-field Survey (SWF).


      0 FSAP04010100                  
        This applies only to Chang et al. (2021) Plan. Sci. J. 2, id.191. Many of the objects were
        not tied to known Hildas. As a result, the orbital parameters were not available and,
        therefore, the phase angle bisector and phase angles could not be calculated. Generally, the
        phase angle for any Hilda group member is <20 degrees.

        Chang 2022b                    This applies to all Chang et al. (2021) Plan. Sci. J. 2,
                                       id.191. Many of the objects were not tied to known Hildas. As
                                       a result, the orbital parameters were not available and,
                                       therefore, the phase angle bisector and phase angles could
                                       not be calculated. Generally, the phase angle for any Hilda
                                       group member is <20 degrees.


      0 Himalia                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


      0 P/2006 HR30                   
        Determined to be a comet after initial discovery and asteroid designation (2006 HR30).
        Current MPC designation is P/2006 HR30.


      0 P0007F                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


      0 P00095                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


      0 P000DV                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000K7                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000ZE                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000ZL                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


      1 Ceres                         
        Drummond 2014                  D_equatorial: 967 ± 10 km; D_polar: 892 ± 10 km.

        AKARI                          This note applies to all 'AKARI' details records. The Usui
                                       (2011) paper (AKARI/IRC Survey) used H values from Lowell
                                       Observatory's ASTORB file and assumed ± 0.05 mag error. In
                                       some cases, using the stated values for albedo and diameter
                                       in the standard formulae to compute H (see LCDB README) does
                                       not give the ASTORB value of H, usually differing by
                                       0.01-0.02 mag.


      2 Pallas                        
        Carry 2010a                    Density = 3.4 ± 0.9 g/cc.  Dimensions: a = 275 ± 4 km; b =
                                       258 ± 3 km; c = 238 ± 3 km.

        Durech 2011a                   This applies to all entries for Durech 2011a. All but 14 of
                                       the spin axis values in Durech 2011a are assumed values taken
                                       from the literature. See the original paper for specifics.

        Hanus 2017b                    Hanus 2017b is based on combining photometric, adaptive
                                       optics, and occulation observations.


      3 Juno                          
        Pravec 2012b                   This note applies to all Pravec 2012b entries. In almost all
                                       cases, the original Pravec values were H_R. The H_V values
                                       were derived using assumed V-R values from various sources
                                       based on known taxonomic class or orbital position. If a
                                       diameter and albedo are given, these are revised values based
                                       on the original WISE H, G, D, and pV, corrected using the new
                                       H-G values and Harris and Harris (1997).

        Pal 2020                       This applies to all records from Pal 2019 Period and
                                       amplitude errors were not included in the original data set.
                                       During the mass import of their results table, the period
                                       error was set to five units of the last decimal place. The
                                       amplitude error was set to 20% of the reported amplitude. The
                                       errors are a general guide only and should not be considered
                                       valid for statisitcal studies unless after reviewing the
                                       original plots. These are available at:
                                       http://archive.konkoly.hu/pub/tssys/dr1/object_plots/


      4 Vesta                         
        Fornasier 2011b                Observations made from Rosetta spacecraft.

        Hasegawa 2014b                 H_B: 3.96 ± 0.01, G_B: 0.30 ± 0.02; H_SZ: 3.08 ± 0.02, G_SZ:
                                       0.25 ± 0.01.


      5 Astraea                       
        Durech 2009                    The pole (126, +40) agrees well with occultation profiles.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


      6 Hebe                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Marsset 2017                   Marsset 2017 combined photometric, adaptive optics, and
                                       occultation data.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


      7 Iris                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


      8 Flora                         
        Torppa 2003                    The sidereal period is believed incorrect (see Durech entry
                                       from DAMIT web site). The pole solution is still in close
                                       agreement with other solutions.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless


      9 Metis                         
        Durech 2011web                 Pole solution verified by Keck AO and occulation
                                       observations.

        Drummond 2012                  Effective diameter derived from ellipsoid of 218x175x129 km.


     10 Hygiea                        
        Durech 2011a                   Second pole solution (312,-42) gives a diameter of 443 ± 45
                                       km. This is not the preferred solution.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     11 Parthenope                    
        Mahlke 2021                    The errors for H, G1, G2 are the larger of the HDI 95% values
                                       given for each parameter. In many cases, there are two
                                       entries for each asteroid, one for the c(yan) and the other
                                       for the o(range) ATLAS filter. The taxonomic class is on the
                                       Bus-DeMeo system was taken from various references. This work
                                       did not determine class independently.


     13 Egeria                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Masiero 2017                   The albedo error given for Masiero 2017 is the maximum
                                       possible value when converting from albedo values from log
                                       space to value space.


     14 Irene                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Colazo 2021d                   This applies to all Colazo 2021d entries. There are up to
                                       three details entries per object: 1) H-G using Gaia GR
                                       magnitudes, 2) H-G with GR magnitudes transformed to V and
                                       adding ground-based data to include phase angles < 10 deg,
                                       and 3) H-G1,G2 using the same magnitudes as in 2. Only
                                       results where there were valid numbers for H and HErr and the
                                       G or G1/G2 errors were <= 1.0 were included in the LCDB
                                       entries. H/HErr were rounded to two decimal places and G/GErr
                                       values were rounded to three decimal places. For a new
                                       summary record, the MPCOrb values are used for H and G for
                                       groups 1 and 3. This provides the necessary consitency for H
                                       when generating frequency-diameter plots from LCDB data,
                                       which have have been historically based on the H(V)-G system.
                                       For the Details record, the H Band is 'GR' for group 1 and
                                       'V' for groups 2 and 3. To help convey that the V magnitudes
                                       were derived from GR and assumed V-R magnitudes, the H Method
                                       is 'D' (Derived). The G Method will be empty for groups 1 and
                                       2 since, regardless

        Martikainen 2021               This applies to all Martikainen 2021 entries (A 649, A98). Of
                                       the 492 asteroids in their tables, only 312 were included in
                                       the LCDB: those where H_G, G1, and G2 were found. They found
                                       that H_G and H_V had a strong 1:1 correlation, i.e., in
                                       almost all cases, the two values were essentially the same.
                                       For the Details records, the taxonomic class given by
                                       Martikainen et al. has a suffix of '(T)' (Tholen) or '(BDM)'
                                       Bus-DeMeo. The phase angle is the average of the min/max
                                       phase angles. The PAB values could not be computed. No errors
                                       were given for G1/G2. They have been assumed to be 0.05.
                                       Since the results are based in part on dense lightcurves, the
                                       Survey flag was set to LCI-D even though sparse Gaia data
                                       were included.


     15 Eunomia                       
        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     16 Psyche                        
        Durech 2011a                   Second pole solution (213,1) has a slightly larger error bar
                                       (36 km) for the diameter.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     17 Thetis                        
        Behrend 2007web                Originally reported P = 12.27 ± 0.05. Updated in 2011.

        Behrend 2011web                Originally reported P = 12.259 ± 0.007 h. Updated in 2011
                                       with additional data.


     19 Fortuna                       
        Durech 2011web                 Pole confirmed by HST and occultation observations.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Veres 2015                     Veres et al. (2015) from Pan-STARRS photometry. The value for
                                       G is G12, not G1, and so the G2 values are NULL.


     21 Lutetia                       
        Belskaya 2010a                 The period given was adopted from work by Faury (2008).

        Carry 2010b                    Shape model is non-convex.

        Durech 2017                    Durech 2017: Combined photometric and thermal data.


     22 Kalliope                      
        Descamps 2008a                 Linus D = 28 ± 2 km. Kalliope a = 117.5, b = 82, c = 62 km.

        Marchis 2008c                  D(Linus) > 22 km

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Stephens 2022c                 Based on data set that combined two observing runs about 10
                                       days apart.


     23 Thalia                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     27 Euterpe                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     28 Bellona                       
        Behrend 2006web                Originally reported as 16.3 h.

        Behrend 2007web                Originally reported as 16.32 h.

        Behrend 2008web                Originally reported as 16.623 h. Modified to fit period found
                                       with 2012 data.

        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     29 Amphitrite                    
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     30 Urania                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     31 Euphrosyne                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     32 Pomona                        
        Behrend 2008web                Originally reported with P = 7.1. Updated in 2011 to fit
                                       period found with 2011 data (11.7 h). Updated in 2016 to fit
                                       period found from 2016 data.

        Behrend 2011web                Originally reported P = 7.1 h. Updated in 2011 to fit period
                                       found from 2011 data. Updated in 2016 to force fit to period
                                       found from 2016 data.

        Behrend 2012web                Originally reported 11.7 h. Changed to force a fit to period
                                       found from 2016 data.


     34 Circe                         
        Durech 2011a                   Second pole (275,51) gives a diameter of 107 ± 10 km. The two
                                       solutions are about equally likely.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     35 Leukothea                     
        Pilcher 2009d                  Pole solution was determined using 'amplitude-aspect' method.


     36 Atalante                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     37 Fides                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     39 Laetitia                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     40 Harmonia                      
        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     41 Daphne                        
        Conrad 2008b                   Discovey of S/2008 (41) 1.

        Matter 2011                    The diameter is based on a non-convex model using lightcurves
                                       and AO images. A convex model gives an effective diameter of
                                       194-209 km.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     42 Isis                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     45 Eugenia                       
        Merline 1999                   Discovery of S/1998 (45) 1

        Marchis 2006c                  Detection of known satellite.

        Marchis 2007                   Discovery of second satellite. D ~ 6 km.

        Hanus 2012a                    Diameter derived from combined LC inversion model and
                                       adaptive optics data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     47 Aglaja                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     50 Virginia                      
        Fornasier 2011a                The taxonomic classes given by Fornasier et al. are on the
                                       Tholen system.


     52 Europa                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Merline 2013a                  Diameter and albedo based on a rocky body. An equally likely
                                       solution assuming a collection of bare rock slabs gives D =
                                       0.004 ± 0.001 km and pV = 0.45 ± 0.35.


     53 Kalypso                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     54 Alexandra                     
        Torppa 2008a                   Sidereal period is for (307,  20) solution.

        Durech 2011a                   The second pole solution (156,13) is the least preferred. It
                                       also gives a different diameter of 135 ± 20 km and sidereal
                                       period of 7.022641 h.

        Durech 2011web                 The pole solution (318, +23) has P_sidereal = 7.022649 h.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     62 Erato                         
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)

        Jiang 2021                     This note applies to all Jiang 2021 entries. The diameter
                                       error is the larger of a two, non-linear error values.


     68 Leto                          
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     69 Hesperia                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     70 Panopaea                      
        Wilawer 2022                   This applies to all Wilawer 2022 (MNRAS 513, 3242-3251): The
                                       observations for each asteroid spanned several months. The
                                       phase and PAB angles are for the first date of the
                                       observations (Zero phase). Period errors were not given and
                                       so assumed to be 2 units of the last decimal place.


     72 Feronia                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     80 Sappho                        
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     81 Terpsichore                   
        Timerson 2010                  The diameter was calculated from the a/b values for the
                                       best-fit ellipse. It represents a minimum value.

        Timerson 2010                  The diameter was calculated from the a/b values for the
                                       best-fit ellipse. It represents a minimum value.


     82 Alkmene                       
        Timerson 2015                  Occultation profile gives ellipsoid of 62.8 ± 0.9 x 55.4 ±
                                       0.9 km. Effecitve diameter is based on area of the ellipse.
                                       The shape supports model 146 on the DAMIT site
                                       (http://astro.troja.mff.cuni.cz/projects/asteroids3D/web.php)
                                       


     83 Beatrix                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     85 Io                            
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     87 Sylvia                        
        Behrend 2012web                Single lightcurve from data spanning two months. The
                                       amplitude, and possibly synodic period, seemed to have
                                       changed over the interval.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Carry 2021                     Multiple lightcurves from 1978-08-30 to 2008-04-01.


     88 Thisbe                        
        Durech 2011a                   The second pole solution (247,50) gives a slightly larger
                                       effective diameter: 220 ± 16 km. This is the least preferred
                                       solution.

        Hanus 2013b                    Diameter is derived from occultation-inversion model for
                                       preferred pole solution, which was reported in a previous
                                       work.


     89 Julia                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     90 Antiope                       
        Merline 2000a                  Discovery of satellite.

        Bartczak 2014                  D1: 80.8 ± 1.8 km. D2: 80.4 ± 1.8 km. Separation: 174 ± 4 km.


     93 Minerva                       
        Torppa 2008a                   Sidereal period is for (49, -40) pole solution.

        Marchis 2009                   Estimated sizes: S1 4km; S2 3 km.

        Behrend 2011web                Originally reported as P = 5.98 ± 0.05 h. Forced in 2012 to
                                       agree with period found using 2012 data.

        Marchis 2011a                  D_MinervaI = 4 ± 2 km. D_MinervaII = 3 ± 1 km. P_Orb(MI) =
                                       57.79 h. P_Orb(MII) = 26.74 h.


     94 Aurora                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


     97 Klotho                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


     99 Dike                          
        Waszczak 2015                  Waszczak (2016) H values are based on G12 system. The G12
                                       value is given instead of G and carries 'G' for the source
                                       flag. The LCDB U value is based on the Waszczak et al.
                                       'relflag' value, with relflag = 0 given U = 1 and relflag = 1
                                       given U = 2


    103 Hera                          
        Wang 2019                      G2: 0.45(1)


    105 Artemis                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    107 Camilla                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Marsset 2016                   Discovery of second satellite.

        Pajuelo 2018a                  Orbital period in binaries table is for S1. S2


    108 Hecuba                        
        Behrend 2005web                Originally reported 19.8 h. Updated in 2016 to fit new
                                       period.


    114 Kassandra                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    119 Althaea                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    121 Hermione                      
        Descamps 2009a                 Pole (4, +13) has P_sidereal = 5.550878 h and is based on
                                       non-convex model.


    125 Liberatrix                    
        Durech 2007                    The pole (280, +74) has P_sidereal = 3.968199 h.


    126 Velleda                       
        Behrend 2011web                Originally reported P = 5.36 ± 0.05 h, A = 0.05 ± 0.01 mag.
                                       Updated in 2011 after additional data obtained.


    128 Nemesis                       
        Doubled period (~78 h) cannot be formally excluded.

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    129 Antigone                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    130 Elektra                       
        Behrend 2001web                Originally reported P = 5.43 h. Data forced to fit period
                                       found in 2011.

        Behrend 2009web                Period originally reported as 5.43 ± 0.01 h.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.

        Yang 2014                      S/2014 (130) 1. Second satellite. Projected separation from
                                       primary approx. 550 km.

        Berdeu 2021                    Discovery of third satellite.


    132 Aethra                        
        Binzel 2019                    MITHNEOS Method: VISNIR This note applies to all Binzel 2019
                                       (2019Icar..324...41B) detail records:  For the MITHNEOS
                                       method,  VIS indicates visible data only.  NIR indicates
                                       near-infrared data only.  VISNIR indicates both. eVISNIR
                                       indicates the visible portion of the spectrum is from the
                                       Eight-Color Asteroid Survey (ECAS, Zellner et al. 1985) sVis
                                       indicates the visible portion of the spectrum is from the
                                       Sloan Digital Sky Survey (SDSS, Ivezic et al. 2001). TAXON
                                       indicates the type is reported in the literature; see the
                                       source listed in the 'Taxon' reference column of the original
                                       file.  For visible data only (VIS), the taxonomic type is
                                       from the Bus classification system (Bus and Binzel 2002). For
                                       visible plus near-infrared data (VISNIR), the taxonomic type
                                       is from the Bus-DeMeo classification system (DeMeo et al.
                                       2009).  '-comp' refers to the broad taxonomic complex. When
                                       multiple taxonomic classes are listed, they are in subjective
                                       order of most likely type first. ':' indicates the assignment
                                       is


    135 Hertha                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    136 Austria                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Durech 2016                    Models from Durech et al. (2016) are posted on the DAMIT web
                                       site.
                                       http://astro.troja.mff.cuni.cz/projects/asteroids3D/web.php


    139 Juewa                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    145 Adeona                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Wang 2018                      Sidereal period for pole (122, -3): 15.0733 h


    146 Lucina                        
        Durech 2009                    The pole (305, -41) has P_sidereal = 18.55390 h.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    152 Atala                         
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    153 Hilda                         
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html

        Warner 2021i                   Model axis ratios (c = 1.0): a/b = 1.14, a/c = 1.4839.


    155 Scylla                        
        Hanus 2018b                    The Hanus 2018b entries include results only if they are
                                       revisions or rejections of previously reported pole
                                       solutions.


    158 Koronis                       
        Erasmus 2020                   This note applies to all Erasmus 2020 (2020ApJS..247...13E)
                                       detail records: Initial bulk data entry assigned U = 2 for a
                                       period probability >= 75 and U = 2- for < 75. The family
                                       class (C or S) was assigned based on which had the higher
                                       probability (if 50, CS was assigned). All family values of
                                       Nysa-Polana were assigned to Nysa family. SWF (Sparse
                                       Wide-field) was assigned to the Survey entry.


    160 Una                           
        Marciniak 2009a                Pole (308, -41) has P_sidereal = 11.03316 h.


    161 Athor                         
        Pilcher 2010b                  Pole solution was determined using 'amplitude-aspect' method.


    165 Loreley                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    167 Urda                          
        Durech 2011a                   The second pole solution (107,-69) gives a slightly larger
                                       effective diameter: 51 ± 15 km. This is the least preferred
                                       solution.


    176 Iduna                         
        Wang 2018                      Sideral period for pole solution (156,+73): 11.29382 h.


    178 Belisana                      
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)


    184 Dejopeja                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    194 Prokne                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    196 Philomela                     
        Durech 2007                    Pole (276, -49) has P_sidereal = 8.332827 h.


    198 Ampella                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    201 Penelope                      
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    202 Chryseis                      
        Behrend 2005web                Originally reported P = 11.8 ± 0.5. Updated in 2011.


    208 Lacrimosa                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    211 Isolda                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    216 Kleopatra                     
        Marchis 2008e                  AO observations show two satellites, ~5 km and ~3 km.
                                       Distances: 650 km and 380 km, respectively.

        Shepard 2018                   DimensionsL 276 x 94 x 178 km


    221 Eos                           
        Hanus 2018a                    Hanus 2018 combined optical photometric and IR (WISE) data
                                       for shape modeling. Shape modeling quality rating (QF) is
                                       from Hanus 2017c.


    224 Oceana                        
        Behrend 2006web                Originally reported P = 18.93 ± 0.05. Updated in 2011.


    228 Agathe                        
        Szabo 2016                     The plots for Szabo 2016a were made available off-line. They
                                       were not included in the original paper or in supplemental
                                       data.


    230 Athamantis                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    238 Hypatia                       
        Behrend 2004web                Originally reported 8.88 h. Updated in 2011.


    239 Adrastea                      
        Behrend 2007web                Originally reported as 19.846 h. Modified based on results
                                       from later observations.


    250 Bettina                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    266 Aline                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    271 Penthesilea                   
        Podlewska-Gaca 2021            This note applies to all Podlewska-Gaca et al. (2021) Ap. J.
                                       Suppl. Ser. 2021, id. 4. The given observation date is the
                                       mid-date for runs C9a and C9b. Few lightcurves were
                                       published. By default, entries from Table 2 were assigned U =
                                       2; entries from Table 3 were rated U = 2-. entries in Table 4
                                       were also given U = 2- with the errors assumed to be 25% of
                                       the listed period.


    275 Sapientia                     
        Dose 2022c                     G values in Dose 2022c were derived by finding the value for
                                       G that gave the lowest RMS fit to the Fourier curve. The
                                       value for G may or may not be consistent with the taxonomic
                                       classification.


    276 Adelheid                      
        Durech 2011a                   The second pole solution (199,-20) gives a slightly smaller
                                       diameter: 117 ± 15 km. The two solutions are about equally
                                       likely.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.
                                       Occultation-inversion gives D = 125 ± 15.


    282 Clorinde                      
        Dose 2023a                     The values for G in Dose 2023 (MPB 50, 65-73) were found by
                                       minimizing the RMS scatter of a Fourier fit, not by strict
                                       calculation.


    283 Emma                          
        Durech 2011web                 Pole (251, +22) has P_sidereal = 6.895222 h.


    298 Baptistina                    
        Carvano 2010                   H_R = 10.92 was directly measured value. The H = 11.30 is the
                                       result of using H_R and V-R = 0.38 measured by the authors.


    302 Clarissa                      
        Durech 2011a                   The first pole solution (28,-72) is preferred.


    306 Unitas                        
        Durech 2011a                   The second pole solution (253,-17) gives a slightly larger
                                       diameter: 53 ± 5. This is the least preferred solution.


    308 Polyxo                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    312 Pierretta                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    317 Roxane                        
        Merline 2009                   Estimated Ds/Dp: 0.26 (based on magnitude differences).


    331 Etheridgea                    
        Warner 2010i                   Presuming the nightly calibrations were correct, the data
                                       provide any number of solutions. If the two sessions are
                                       forced to overlay, a number of solutions, less than 24 h, are
                                       still possible.


    345 Tercidina                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    349 Dembowska                     
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    350 Ornamenta                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    352 Gisela                        
        Erasmus 2020                   This note applies to all Erasmus 2020 (2020ApJS..247...13E)
                                       detail records: Initial bulk data entry assigned U = 2 for a
                                       period probability >= 75 and U = 2- for < 75. The family
                                       class (C or S) was assigned based on which had the higher
                                       probability (if 50, CS was assigned). All family values of
                                       Nysa-Polana were assigned to Nysa family. SWF (Sparse
                                       Wide-field) was assigned to the Survey entry.


    354 Eleonora                      
        Behrend 2001web                Originally reported P = 4.3 ± 0.1. Updated in 2011 to fit
                                       data to a period found with a different data set.

        Behrend 2002web                Originally reported P = 4.282 ± 0.005, A = 0.52 ± 0.02.
                                       Updated in 2011.

        Behrend 2006web                Originally reported P  = 4.27750 ± 0.00003 h, A = 0.20 ±
                                       0.01. Updated in 2011.

        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    355 Gabriella                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    362 Havnia                        
        Wang 2015b                     Period for second pole is 16.918935 ± 0.000043 h.


    370 Modestia                      
        Athanasopoulos 2022            The orginal paper reported a pole of (268, -92).  |Latitude|
                                       > 90 deg is not allowed in LCDB. In such a case, 180 deg is
                                       added to or subtracted from the longitude and the
                                       complimentary latitude is used. In this case, that means
                                       latitude = -88 deg.


    372 Palma                         
        Durech 2011a                   The second pole solution (44,17) gives a different diameter
                                       (198 ± 26 km) and sidereal period (8.58191 h). The two
                                       solutions are about as likely.


    374 Burgundia                     
        Behrend 2018web                Two halves of 13-h period are identical, leaving half-period
                                       a distinct possibility.


    382 Dodona                        
        Behrend 2021web                The two earliest observation runs were ignored in assigning
                                       the U code. They are what appear to be obvious outliers.


    386 Siegena                       
        Behrend 2004web                Period originally reported as 7.6 h.


    390 Alma                          
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    391 Ingeborg                      
        Binzel 2019                    MITHNEOS Method: VIS


    394 Arduina                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    409 Aspasia                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.
                                       Occultation-inversion gives D = 173 ± 17 km.


    414 Liriope                       
        Chang 2015                     Chang (2015) H values are based on H-G system. The G values
                                       are in R, not V. All lightcurves rated U=2-3 by Chang were
                                       reviewed and a formal U code was assigned by the LCDB
                                       authors. The objects in their U = 1 list were all given U =
                                       1.


    418 Alemannia                     
        Gorby 2018                     Results table has incorrect period.


    423 Diotima                       
        Hanus 2013b                    Diameter is derived from AO-inversion model for preferred
                                       pole solution, which was reported in a previous work.


    433 Eros                          
        Trilling 2010                  The Trilling (2010) results are based on using values for H
                                       taken from the JPL Horizons site. In Trilling (2010), there
                                       is often a significant disagreement among the albedo,
                                       diameter, and H values when they are applied to the standard
                                       formula that relates these three values (see LCDB README
                                       file), i.e., using the Trilling albedo and diameter values
                                       gives a differnt value for H than stated, sometimes by up to
                                       0.1 mag.

        Mueller 2011a                  H and G taken from other sources.

        Thomas 2011b                   This note applies to all entries for Thomas 2011b. Warm
                                       Spitzer observations. The error is the larger of the + or -
                                       (which were not the same).

        Binzel 2019                    MITHNEOS Method: VISNIR


    434 Hungaria                      
        Morrison 1979                  Morrison values were based on V(1,0) magnitude system. They
                                       have been converte

        Lucas 2017                     The Lucas 2017 taxonomic classifications are on the Bus-DeMeo
                                       system.

        Wang 2021                      This applies to all Wang & Xu (2021). The pole coordinates
                                       and sidereal period uncertanties were not specified. Default
                                       errors for longitude and latitude of ± 10 deg were used while
                                       the default period error used was 2 units in the last decimal
                                       place.


    435 Ella                          
        Chang 2016                     Chang (2016) H values are based on H-G system. The G values
                                       are in R, not V. All lightcurves with a period were initially
                                       given U = 2 regardless of rating by Chang et al. The plots
                                       for the 352 lightcurves that did not have complete coverage
                                       were reviewed and the U codes revised. In many of those
                                       cases, it appears that the half-period was found. For those,
                                       if the summary line depended on the Chang et al. entry, the
                                       period on the summary line is double that found by Chang et
                                       al. and carries a 'D' (determined) flag in the NOTES field.
                                       No errors were given for amplitudes, which were often
                                       dramatically overstated.


    437 Rhodia                        
        Behrend 2005web                Originally reported 52.8 h. Updated to fit period found with
                                       2016 data.


    444 Gyptis                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    469 Argentina                     
        Wang 2003                      BIN: Reported possibility of being binary.      Considered
                                       unreliable.

        Wang 2005                      NPA: Reported secondary period of 8.74 hr.       Considered
                                       unreliable.


    470 Kilia                         
        Pilcher 2020f                  Second period of 119.3 h in lc_npar is one of several
                                       possibilities.


    471 Papagena                      
        Torppa 2008a                   Sidereal period is for (29, 41) solution.


    475 Ocllo                         
        Binzel 2019                    MITHNEOS Method: TAXON


    479 Caprera                       
        Behrend 2002web                Originally reported P = 5.259 ± 0.002 h, A = 0.34 ± 0.09 h.
                                       Updated in 2011 to fit data to a new period found with a
                                       different data set.

        Behrend 2004web                Originally reported P = 5.247 ± 0.006 h, A = 0.08 ± 0.01 mag.
                                       Updated in 2011 to fit to a new period found from a different
                                       data set.

        Behrend 2007web                Originally reported P = 5.2491 ± 0.0002, A = 0.07 ± 0.01 mag.
                                       Updated in 2011 to fit data a new period found with a
                                       different data set.


    488 Kreusa                        
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    506 Marion                        
        Wang 2015b                     Period for second pole solution is 16.549751 ± 0.000060


    511 Davida                        
        Conrad 2007                    Measured ellipsoid (a,b,c): 357±2, 294±2, 231±50 km.


    512 Taurinensis                   
        Binzel 2019                    MITHNEOS Method: VISNIR


    522 Helga                         
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    531 Zerlina                       
        Behrend 2002web                Originally reported 7.2 h. Updated to fit period found with
                                       2016 data.


    540 Rosamunde                     
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    544 Jetta                         
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    550 Senta                         
        Behrend 2004web                Originally reported 19.584 h. Updated to fit period found in
                                       2016.

        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    566 Stereoskopia                  
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    585 Bilkis                        
        Wang 2016                      All lightcurves for Wang et al. 2016 were forced to sidereal
                                       period and were in intensity units of the inversion model
                                       curve, therefore there were no amplitudes in magnitude given.
                                       


    588 Achilles                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


    617 Patroclus                     
        Buie 2015                      Volume equivalent diameters based on derived ellipsods are
                                       D_Patroclus: 113 km; D_Menoetius: 104 km

        Chatelain 2016                 The B-V and V-R magnitudes for the Chatelain 2016 (Icarus
                                       271) were derived from the data table in Appendix A. The
                                       median errors for these color indexes in the paper are given,
                                       not the actual values for the individual results. The B-R and
                                       V-I magnitudes are from Table 3. The B-V and V-R values may
                                       not yield the exact numbers of the stated B-R and V-I
                                       magnitudes.

        Berthier 2020                  Area-equivalent diameter.


    624 Hektor                        
        The objects under Sonnett 2015 were observed in the W3 (12 um) band by WISE. The amplitude
        given is the maximum range of values, not the range of a fitted lightcurve. No periods were
        given for the data.


    636 Erika                         
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    654 Zelinda                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    676 Melitta                       
        Behrend 2002web                Originally reported as 8.5734.

        Behrend 2006web                Originally reported as 14.09 h.


    694 Ekard                         
        Timerson 2010                  A least squares fit to the irregular shape derived from the
                                       occultation observations and based on a shape model by Torppa
                                       et al. (2003) yields the stated diameter.

        Timerson 2010                  A least squares fit to the irregular shape derived from the
                                       occultation observations and based on a shape model by Torppa
                                       et al. (2003) yields the stated diameter.


    699 Hela                          
        Behrend 2003web                Originally reported 4.765 h. Updated to fit period found with
                                       2016 data.

        Binzel 2019                    MITHNEOS Method: VISNIR


    702 Alauda                        
        Rojo 2011                      R_orbit = 1230 km.


    704 Interamnia                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    719 Albert                        
        Binzel 2019                    MITHNEOS Method: VISNIR


    727 Nipponia                      
        Baxter 2019                    Baxter et al. (2019) also reported shape models for each
                                       asteroid in their paper, but did not give the sidereal period
                                       or pole solution.


    728 Leonisis                      
        Galad 2010c                    The lightcurves from Galad 2010c are based on data from the
                                       SDSS Moving Object Catalog.


    763 Cupido                        
        Pilcher 2018d                  Ambiguous second period. Other possibility is 121 h.


    777 Gutemberga                    
        Polakis 2018d                  The ambiuous table includes the half-period for this work.
                                       However, given the amplitude and low phase angle, the LCDB
                                       authors chose not to include the 'A' flag in the Notes field
                                       of this record or the summary line.


    786 Bredichina                    
        Dose 2021b                     The period/amplitude given in results table are significantly
                                       different from those in the plot. The latter were close to
                                       previous results and so adopted for this entry.


    809 Lundia                        
        Marchis 2012                   Hv assumed V-R = 0.54.

        Bartczak 2017                  Reported pole is the pole of the orbit for the fully
                                       syncrhonous binary. Amplitudes are for out of eclipse
                                       lightcurve.


    825 Tanina                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    853 Nansenia                      
        Behrend 2001web                Originally reported P = 9.31 h. Update in 2011 based on a new
                                       period but the solution is still highly ambiguous.


    854 Frostia                       
        Marchis 2012                   Hv assumed V-R = 0.54.


    887 Alinda                        
        Morrison 1974                  Morrison gives D = 5. in his table as well as log(D). The
                                       latter results in a value of 5.2 km. We used the latter.

        Dunlap 1979                    The authors give H_v(1,0) = 14.10 ± 0.08. For conversion to
                                       the current H-G system, we use Ho = H(1,0) - 0.34.

        Binzel 2019                    MITHNEOS Method: eVISNIR

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


    901 Brunsia                       
        Wisniewski 1997                A period of 3.139 h (with bimodal curve) was also found by
                                       Wisniewski but the final paper adopted the triply-periodic
                                       value of 4.872 h.


    911 Agamemnon                     
        Timerson 2013                  Ds = 3-10 km. Based on single video observation.


    925 Alphonsina                    
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    939 Isberga                       
        Carry 2015                     D1: 12.4 ± 2.5 km; Ds: 3.6 ± 0.7 km


    951 Gaspra                        
        Thomas 1994                    Diameter is mean radius of irregular object with principal
                                       diam

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


    966 Muschi                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


    987 Wallia                        
        Behrend 2008web                Period originally reported as 7.0 h.


   1011 Laodamia                      
        Apostolovska 2014              a/b: 0.83; b/c: 1.3

        Binzel 2019                    MITHNEOS Method: VISNIR


   1016 Anitra                        
        Pilcher 2016f                  Orbital period an approximate estimate based on four possible
                                       mutual events. First entry (Date: Nov 8, 2015) is for full
                                       data set covering three months. Subsequent entries are based
                                       on subsets.


   1036 Ganymed                       
        Velichko 2012                  Obs date estimated from phase angle given in paper.

        Velichko 2013                  Ellipsoid lengths: a = 960 km, b = 770 km, c = 495 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1052 Belgica                       
        Franco 2013b                   Ds/Dp >= 0.36 ± 0.02

        Franco 2013c                   Ds/Dp = 0.36 ± 0.02

        Franco 2020e                   The original paper gives Ds/Dp > 0.34. The 0.16 mag
                                       attenuation gives closer to 0.39. The latter is given in the
                                       lc_binaries table.


   1055 Tynka                         
        Behrend 2012web                Originally reported as P = 12.8 ± 0.5 h.

        Fornas 2023a                   Stepehens data (ALCDEF, 2012 Mar-May) included for analysis.


   1061 Paeonia                       
        Pilcher 1987                   Pilcher's notes for 1986 Dec. 4 show observations form
                                       4:20-8:00 UT with fading by about 0.5 magnitude 5:10-7:00 UT,
                                       then brightening by 8:00.  For 1986 Dec. 5, 1061 Paeonia was
                                       'fairly easy at 5:20, 6:15, invisible at 7:20, dimly seen
                                       again 8:05 at lower altitude.


   1065 Amundsenia                    
        Binzel 2019                    MITHNEOS Method: VIS


   1069 Planckia                      
        Behrend 2006web                Originally reported P = 11. h, A = 0.18. Updated in 2011 to
                                       fit data to new period.


   1070 Tunica                        
        Waszczak (2015) H values are based on G12 system. The G12 value is given instead of G and
        carries 'G' for the source flag. The G2 value is NUL. The LCDB U value is based on the
        Waszczak et al. 'relflag' value, with relflag = 0 given U = 1 and relflag = 1 given U = 2


   1082 Pirola                        
        Baker 2011a                    When using maximum light, H = 10.320 ± 0.013, G = 0.107 ±
                                       0.016.


   1089 Tama                          
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Behrend 2011web                Originally reported P = 16.45 ± 0.05, A = 0.12 ± 0.02 mag.
                                       Updated in 2011 with additional data.


   1095 Tulipa                        
        Behrend 2005web                Originally reported P = 2.78730 ± 0.00005 h, A = 0.20 ± 0.01
                                       mag. Updated in 2011.


   1100 Arnica                        
        Slivan 2008                    A footnote to Table 2 in the Slivan et al. (2008) paper
                                       indicates that subsquent data (not included in the paper)
                                       show the period to be 14.535 h instead of the ~29 h reported
                                       in the paper. The 2007 data were not plotted in the paper.


   1131 Porzia                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1134 Kepler                        
        Binzel 2019                    MITHNEOS Method: VIS


   1139 Atami                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1152 Pawona                        
        Wang 2022                      Sidereal period for (162, 58) and (323, 61): 3.41437 h.


   1170 Siva                          
        Binzel 2019                    MITHNEOS Method: TAXON


   1183 Jutta                         
        Erasmus 2021                   This note applies to all Erasmus et al. (2021, MNRAS). The Hv
                                       from JPL is generally within Â±0.3 mag of the ATLAS H_c
                                       values reported in the paper. The C/S taxonomic class is
                                       dervived from the color indices and express as a probability.
                                       For the LCDB entries, objects >= 66% of C or S are assigned a
                                       single letter. Otherwise, C/S is listed.


   1188 Gothlandia                    
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.

        Baker 2012a                    Using maximums of lightcurves, the authors found H = 11.425 ±
                                       0.014 and G = 0.230 ± 0.015. Diameter and albedo are
                                       revisions to WISE values applying the author's H-G and Harris
                                       and Harris (1997) correction.


   1198 Atlantis                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1204 Renzia                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1207 Ostenia                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1268 Libya                         
        Warner 2023e                   Primary period (14.11) not ambiguous but there is a secondary
                                       period of 5.04 h that improves the primary lightcurve fit
                                       considerably but may not have a physical cause.


   1270 Datura                        
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1278 Kenya                         
        Oey 2012b                      The second tumbling period of 127 h is a likely but not
                                       definitive candidate.


   1293 Sonja                         
        Binzel 2019                    MITHNEOS Method: VIS


   1310 Villigera                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


   1313 Berna                         
        Marchis 2012                   Hv assumed V-R = 0.54.


   1316 Kasan                         
        Binzel 2019                    MITHNEOS Method: VIS


   1333 Cevenola                      
        Marchis 2012                   Hv assumed V-R = 0.54.


   1346 Gotha                         
        Behrend 2006web                Originally reported P = 2.6540 ± 0.0003 h.


   1374 Isora                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1406 Komppa                        
        Behrend 2011web                Authors reported P = 7.02 with 4 max/min.


   1428 Mombasa                       
        Stephens 2012web               A half-period of 8.38 h cannot be formally excluded.


   1443 Ruppina                       
        Stephens 2020e                 axis ratios (c=1): a/b: 1.291, a/c: 1.210


   1453 Fennia                        
        Warner 2016i                   To find the primary period, the satellite orbital period was
                                       forced to near previous results.


   1468 Zomba                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   1474 Beira                         
        Binzel 2019                    MITHNEOS Method: TAXON


   1489 Attila                        
        Chang 2019a                    This note applies to all Chang 2019 (ArXiv:1901.08719) detail
                                       records: The U code reported in Chang et al. is not
                                       necessarily the LCD value. Initial bulk data entry assigned U
                                       = 2 pending individual review. Amplitude errors were not
                                       given. A default of 10% of the amplitude was assigned pending
                                       individual review


   1499 Pori                          
        Behrend 2008web                Originally 3.36 h. Updated to fit period found in 2016.


   1508 Kemi                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1509 Esclangona                    
        Merline 2003a                  Ds ~4 km. Distance from Primary: 140 km.

        Marchis 2012                   Hv assumed V-R = 0.54.


   1512 Oulu                          
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   1514 Ricouxa                       
        Durech 2009                    Ambiguous pole solution. The longitude is unknown and the
                                       beta is an average of several solutions with the error being
                                       the dispersion.


   1536 Pielinen                      
        Casalnuovo 2016                Secondary period P = 6.43 ± 0.01 h reported. Likely harmonic
                                       of main period.


   1565 Lemaitre                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1566 Icarus                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1580 Betulia                       
        Binzel 2019                    MITHNEOS Method: sVISNIR


   1593 Fagnes                        
        Binzel 2019                    MITHNEOS Method: VIS


   1620 Geographos                    
        Durech 2008b                   Pole/period in spin axis table are for 1969 January 7.5. YORP
                                       acceleration found.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Durech 2022                    YORP parameter: 1.14(03)*(10^-8 rad d^-2)


   1627 Ivar                          
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1640 Nemo                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1656 Suomi                         
        Franco 2022d                   Unexplained attenuation on 2022 May 18.


   1667 Pels                          
        Stephens 2020e                 axis ratios (c=1): a/b:1.247m a/c: 1.135


   1685 Toro                          
        Binzel 2019                    MITHNEOS Method: VISNIR

        Durech 2022                    YORP Parameter: 0.33(3) * (10^-8 rad d^-2)


   1723 Klemola                       
        Behrend 2005web                Originally reported P = 6.22 h. Updated in 2011 to fit period
                                       found with 2011 data.


   1727 Mette                         
        Behrend 2003web                Period originally reported as 2.982 ± 0.002 h.

        Behrend 2006web                Originally reported as P = 2.98141 ± 0.00005 h.

        Warner 2013i                   Ds/Dp: >= 0.20 ± 0.02. Unusual because primary is moderately
                                       elongated, a/b = 1.36:1 assuming equatorial view of triaxial
                                       ellipsoid.

        Warner 2013l                   Ds/Dp = 0.21 ± 0.02

        Warner 2016l                   Orbital period forced to range near previous results. As
                                       stand-alone data set, insufficient evidence to suggest a
                                       satellite.


   1741 Giclas                        
        Pravec 2019b                   Paired with (258640) 2002 ER36. This note applies to all
                                       Pravec 2019b:  Albedos were not reported. They were
                                       calculated based on the H and Diameter given in the paper.
                                       This was done to allow comparing the albedo required to match
                                       the given values against the albedo given in the summary
                                       and/or other detail records.


   1747 Wright                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1770 Schlesinger                   
        Pravec 2016web                 Orbital periods for 2016 have no real meaning. They were used
                                       to demonstrate behavior of lightcurve data beyond primary
                                       lightcurve. The 2015 secondary period could be independent
                                       rotation of the satellite or signs of a third member.


   1777 Gehrels                       
        Pravec 1990web                 Reanalysis of the Wisniewski data.


   1778 Alfven                        
        Chang 2014a                    This note applies to all entries from Chang et al. (2014, ApJ
                                       788, A17) where they used 2nd order Fourier fits This
                                       produced amplitudes that didn't necessarily fit the data. The
                                       amplitudes in the LCDB were determined by the LCDB authors.
                                       In some cases, the precision of the period was considered too
                                       high and rounded to the nearest 0.1 h while in other cases,
                                       the stated period was converted to a >X h estimate.


   1829 Dawson                        
        Galad 2010c                    Combined with data from Pray (2006a)


   1830 Pogson                        
        Pravec 2012a                   D2/D1 = 0.28 ± 0.02. Value of D2/D1 = 0.30 ± 0.02 was adopted
                                       as mean of data from three apparitions.

        Pravec 2012a                   Asynchronous status assigned to satellite generating mutual
                                       events.

        Fauerbach 2019e                The known secondary period of 3.2626 h was used to extact the
                                       primary rotation period.


   1850 Kohoutek                      
        Chang (2016) H values are based on H-G system. The G values are in R, not V. All lightcurves
        with a period were initially given U = 2 regardless of rating by Chang et al. The plots for
        the 352 lightcurves that did not have complete coverage were reviewed and the U codes
        revised. In many of those cases, it appears that the half-period was found. For those, if
        the summary line depended on the Chang et al. entry, the period on the summary line is
        double that found by Chang et al. and carries a 'D' (determined) flag in the NOTES field. No
        errors were given for amplitudes, which were often dramatically overstated.


   1862 Apollo                        
        Kaasalainen 2007               Period is for zero-epoch of November 13, 1980. Paper proved
                                       spin up due to YORP effect.

        Rozitis 2013                   The authors assumed the pole and sidereal period from
                                       previous works to derive the required diameter and albedo to
                                       fit a thermophysical model that accuratly predicts Yarkovsky
                                       and YORP rates of change.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1863 Antinous                      
        Masiero 2017                   The albedo error given for Masiero 2017 is the maximum
                                       possible value when converting from albedo values from log
                                       space to value space.

        Binzel 2019                    MITHNEOS Method: VIS


   1864 Daedalus                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Masiero 2020a                  This note applies to all entries for Masiero et al. (2020a).
                                       The albedo error is the listed maximum possible value when
                                       converting albedo values from log space to value space. The
                                       phase angle in the details record is from the file since the
                                       actual date of observation was not given. The value for H is
                                       the 'model-out' value, which may differ slightly from the
                                       value used in the NEATM modeling (the value given in Tables
                                       1-4). This maintains full agreement with the listed albedo
                                       and diameter. See Masiero et al. (2020a) for details about
                                       assumed errors in H and G.


   1865 Cerberus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   1866 Sisyphus                      
        Benner 1985                    Ds/Dp ~ 0.1

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1876 Napolitania                   
        Warner 2016b                   Suspected wide binary where primary has long period and large
                                       amplitude and the satellite has a short period and low
                                       amplitude.


   1915 Quetzalcoatl                  
        Binzel 2019                    MITHNEOS Method: TAXON


   1916 Boreas                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   1917 Cuyo                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1937 Locarno                       
        Behrend 2019web                Reported period 53.6 h but given amplitude and phase, the
                                       double period is more likely.


   1943 Anteros                       
        Mueller 2011a                  H and G taken from other sources.

        Binzel 2019                    MITHNEOS Method: VISNIR


   1947 Iso-Heikkila                  
        Galad 2010c                    For Galad 2010c entries, a compromise date of 2005 Oct 5 was
                                       used to compute phase and PAB for those objects based on SDSS
                                       data where no specific date information was provided.


   1951 Lick                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   1979 Sakharov                      
        Pravec 2011web                 Some suspected events seen but there was no consisetent
                                       solution for a secondary period.


   1980 Tezcatlipoca                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   1981 Midas                         
        Binzel 2019                    MITHNEOS Method: VISNIR

        McGlasson 2022                 A shape was reported (4x2x2) with one lobe being 30% larger.
                                       The neck joining the two lobes is about 60% of the width of
                                       the lobes.


   2006 Polonskaya                    
        Pray 2005c                     Second period due to 1) asynchronous single satelltie or 2)
                                       second satellite.


   2020 Ukko                          
        Pilcher 2015i                  Alternation solutions with bimodal and trimodal solutions are
                                       considered unlikely.


   2030 Belyaev                       
        The errors for H, G1, G2 are the larger of the HDI 95% values given for each parameter. In
        many cases, there are two entries for each asteroid, one for the c(yan) and the other for
        the o(range) ATLAS filter. The taxonomic class is on the Bus-DeMeo system was taken from
        various references. This work did not determine class independently.


   2059 Baboquivari                   
        Masiero 2021                   This note applies to all entries for Masiero et al. (2021;
                                       Plan. Sci. J. 2, A162). The albedo error is the listed
                                       maximum possible value when converting albedo values from log
                                       space to value space. The phase angle in the details record
                                       is from the file since the actual date of observation was not
                                       given. The value for H is the 'model-out' value, which may
                                       differ slightly from the value used in the NEATM modeling
                                       (the value given in Tables 1-4). This maintains full
                                       agreement with the listed albedo and diameter. No specific
                                       errors for H and G were given. Default values of H_err = 0.05
                                       and G_err = 0.1 were used.


   2060 Chiron                        
        Belskaya 2010b                 To derive H, used V-R=0.36 and phase coefficient (not G) of
                                       0.06 mag/degree.

        Belskaya 2015                  The Belskaya et al. (2015) provides updated color index
                                       values for TNOs based on numerous references. See that paper
                                       for the original references.

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


   2061 Anza                          
        Binzel 2019                    MITHNEOS Method: TAXON


   2062 Aten                          
        Binzel 2019                    MITHNEOS Method: NIR


   2063 Bacchus                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2064 Thomsen                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2074 Shoemaker                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   2077 Kiangsu                       
        Binzel 2019                    MITHNEOS Method: sVIS


   2078 Nanking                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   2099 Opik                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   2100 Ra-Shalom                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   2102 Tantalus                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Rozek 2022                     Radar did not detect a satellite D > 75 m, which leaves
                                       earlier reports of a secondary period unexplained.


   2110 Moore-Sitterly                
        Pravec 2019b                   Paired with (44612) 1999 RP27.


   2121 Sevastopol                    
        Sokova 2019                    Orbital period for retrograde solution: 37.153 Ãƒâ€šÃ‚Â±
                                       0.001 h.


   2178 Kazakhstania                  
        Benishek 2018m                 Secondary has lightcurve amplitude of 0.02 mag;


   2201 Oljato                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   2204 Lyyli                         
        Binzel 2019                    MITHNEOS Method: VIS


   2207 Antenor                       
        Stephens 2018k                 Orbital period is Binaries table is one of several solutions.


   2212 Hephaistos                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   2242 Balaton                       
        Marchini 2016b                 Estimated Ds/Dp is a minimum.


   2253 Espinette                     
        Binzel 2019                    MITHNEOS Method: VIS


   2312 Duboshin                      
        Warner 2023e                   P = 51.72 has significant secondary period of P2 = 19.58 h,
                                       A2 = 0.30. The two may be harmonically related (3:8 ratio).


   2320 Blarney                       
        Bennefeld 2009b                The Pal et al. result of 5.99 h is considered highly secure.
                                       The periods are close to a 7:6 ratio and the data from
                                       Bennefield will fit 5.99 h.

        Behrend 2020web                The Pal et al. result of 5.99 h is considered highly secure.
                                       The periods are close to a 14:13 ratio and the data from
                                       Behrend will fit 5.99 h.


   2329 Orthos                        
        Binzel 2019                    MITHNEOS Method: VIS


   2335 James                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   2340 Hathor                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   2343 Siding Spring                 
        Pollock 2015b                  Secondary period in binary report attributed to third body.


   2368 Beltrovata                    
        Binzel 2019                    MITHNEOS Method: TAXON


   2384 Schulhof                      
        Vokrouhlicky 2016b             V-R = 0.49 ± 0.05 assumed. H_R = 11.64 ± 0.03.


   2423 Ibarruri                      
        Binzel 2019                    MITHNEOS Method: VIS


   2449 Kenos                         
        Binzel 2019                    MITHNEOS Method: eVISNIR


   2453 Wabash                        
        Galad 2010c                    Combined with data from Pray (2006c)


   2462 Nehalennia                    
        Szabo 2016 entries are based on Kepler 2 data. Most objects did not have a reported
        period/amplitude.


   2483 Guinevere                     
        The objects under Sonnett 2015 were observed in the W3 (12 um) band by WISE. The amplitude
        given is the maximum range of values, not the range of a fitted lightcurve. No periods were
        given for the data.


   2500 Alascattalo                   
        Bentz 2023                     Period using V data. R data gave P = 2.786(0.050), A =
                                       0.18(0.02).


   2575 Bulgaria                      
        Athanasopoulos 2022            Paper gave Beta1 = 91, which is not allowed in LCDB, so a
                                       value of 90 was entered.


   2577 Litva                         
        Warner 2009q                   P2 is assumed to be due to the rotation of the secondary.
                                       There is slight evidence that the secondary may be tidally
                                       locked and, therefore, P2 is due to the rotation of a third
                                       body in the system.

        Merline 2013b                  P_Orb(S2): 214 d (107 d). D(S2): 1.2 km.

        Merline 2013c                  P_Orb(S2): 214 d (107 d). D(S2): 1.2 km. D(S1): 1.4 km.

        Binzel 2019                    MITHNEOS Method: VIS


   2608 Seneca                        
        Binzel 2019                    MITHNEOS Method: TAXON


   2629 Rudra                         
        Binzel 2019                    MITHNEOS Method: VIS


   2691 Sersic                        
        Oey 2016a                      No mutual events seen but second period found. See binary
                                       data table.


   2712 Keaton                        
        This note applies to all Chang 2019 (ArXiv:1901.08719) detail records: The Chang et al. U
        codes are not necessarily those given in the LCDB. Initial bulk data entry assigned U = 2
        pending individual review.


   2744 Birgitta                      
        Binzel 2019                    MITHNEOS Method: VIS


   2754 Efimov                        
        Pray 2006g                     Ds/Dp = 0.20 ± 0.03.


   2760 Kacha                         
        Warner 2021b                   Weak secondary period of 15.63 h, 0.04 mag provided better
                                       fit but is likely an artifcat of the Fourier anlayis.


   2802 Weisell                       
        Behrend 2006web                Originally reported as P = 37.74 ± 0.06 h, A = 0.41 ± 0.03
                                       mag. Data forced to fit period found in 2011.


   2815 Soma                          
        Pollock 2011                   Ds/Dp = 0.25 ± 0.02.


   2847 Parvati                       
        Behrend 2018web                Overlooked binary?


   2867 Steins                        
        Jorda 2008                     Lightcurve data obtained by OSIRIS/Rosetta spacecraft. The
                                       phase angle was 41.7 as seen from the craft, not the Earth.

        Lamy 2008a                     Axis ratios: a/b: 1.17; a/c: 1.25. Size: 5.73 ± 0.52, 4.95 ±
                                       0.45, 4.58 ± 0.41 km

        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   2881 Meiden                        
        Polakis 2017a                  The assignment of the primary and secondary periods may be
                                       reversed, i.e., the longer of the two periods may be the
                                       primary. The rotation of the satellite responsible for events
                                       is locked to the orbital period.


   2897 Ole Romer                     
        Pravec 2019b                   Paired with (182259) 2001 FZ185.


   2937 Gibbs                         
        Warner 2019r                   Second period found but cause not established. Could be a
                                       tumbler or binary without mutual events.

        Warner 2019r                   The U = 3- rating is for the primary period, which is clearly
                                       established (unless the object is a low-level tumbler).


   2968 Iliya                         
        Binzel 2019                    MITHNEOS Method: sVIS


   3025 Higson                        
        Behrend 2010web                Originally reported 10.8 h. Updated to fit to period found
                                       with 2016 data.


   3040 Kozai                         
        Binzel 2019                    MITHNEOS Method: VIS


   3073 Kursk                         
        Skiff 2019b                    Lightcurve forced to near primary period of known binary and
                                       shows effects of satellite events.


   3102 Krok                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3103 Eger                          
        Durech 2012                    YORP acceleration: (1.4 ± 0.6) x 10^-8 rad d^-2

        Binzel 2019                    MITHNEOS Method: VISNIR


   3122 Florence                      
        Benner 2017                    P_ORB_Inner: ~8h. P_ORB_Outer: ~24h. Satellites are assumed
                                       to be tidally locked to orbital period.

        Binzel 2019                    MITHNEOS Method: VISNIR


   3138 Ciney                         
        Hills 2014a                    Author reported P = 56.1 h with monomodal lightcurve but 0.56
                                       mag amplitude virtually assures a bimodal curve and,
                                       therefore, double period.


   3157 Novikov                       
        Marchini 2019c                 The period in the work was 9.952 h. However, analysis of the
                                       data by the LCDB authors found that 14.930 h was more likely
                                       correct.


   3198 Wallonia                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3199 Nefertiti                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3200 Phaethon                      
        Ansdell 2014                   Color index values are the average of three values derived
                                       over several years. The errors were added in quadrature.

        Radar Team 2017c               Diameter based on high-res (75m/pixel) images.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Tabeshian 2019                 H-G_B: 14.57(2), 0.00(1); H-G_R:13.28(2),-0.10(1); H-G_I:
                                       13.07(2), -0.08(1).


   3250 Martebo                       
        Alvarez 2014b                  Author found H_R = 10.84. A V-R = 0.38 was assumed to give
                                       H_V = 11.22 ± 0.06.


   3255 Tholen                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3260 Vizbor                        
        Diameter and albedo taken from Warner 2012, which revised WISE diameter and albedo with new
        H-G and Harris and Harris (1997).


   3267 Glo                           
        Binzel 2019                    MITHNEOS Method: VIS


   3287 Olmstead                      
        Binzel 2019                    MITHNEOS Method: VIS


   3288 Seleucus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3309 Brorfelde                     
        Warner 2009i                   Ds/Dp: 0.26 ± 0.02


   3343 Nedzel                        
        Binzel 2019                    MITHNEOS Method: VIS


   3352 McAuliffe                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3361 Orpheus                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   3362 Khufu                         
        Binzel 2019                    MITHNEOS Method: VIS


   3401 Vanphilos                     
        Binzel 2019                    MITHNEOS Method: VIS


   3402 Wisdom                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3443 Leetsungdao                   
        Binzel 2019                    MITHNEOS Method: VIS


   3481 Xianglupeak                   
        Pravec 2012web                 A single suspect attentuation was seen.


   3494 Purple Mountain               
        Cantu 2016                     Authors adopted shorter (monomodal) period. However, the
                                       amplitude and phase angle dictated a bimodal solution at the
                                       longer period.


   3548 Eurybates                     
        Noll 2020a                     Obs date is for first detection.


   3551 Verenia                       
        Binzel 2019                    MITHNEOS Method: TAXON


   3552 Don Quixote                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   3553 Mera                          
        Binzel 2019                    MITHNEOS Method: NIR


   3554 Amun                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3581 Alvarez                       
        Binzel 2019                    MITHNEOS Method: VIS


   3623 Chaplin                       
        Marchis 2012                   Hv assumed V-R = 0.54.


   3635 Kreutz                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   3669 Vertinskij                    
        Behrend 2020web                Period matches orbital period of satellite (Christmann et al.
                                       2020; CBET 4749).


   3671 Dionysus                      
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


   3673 Levy                          
        Pravec 2007web                 Refinements on the original parameters reported by Pray et al
                                       in CBET 1165.


   3674 Erbisbuhl                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   3691 Bede                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   3704 Gaoshiqi                      
        Pravec 2010web                 Systematic residuals seen, possibly due to another lightcurve
                                       component, but no good solution could be found.


   3737 Beckman                       
        Binzel 2019                    MITHNEOS Method: VIS


   3749 Balam                         
        Merline 2002a                  Estimated size of satellite: 1.5 km.

        Marchis 2008b                  This is a trinary system, with a more distant satellite
                                       reported via AO observations (2002, IAUC 7827)

        Behrend 2014web                Lightcurve shows mutual events (Amp_max = 0.46 ± 0.03) but
                                       rotation of primary not isolated.

        Pravec 2019b                   Paired with (312497) 2009 BR60.

        Pravec 2019b                   Binary information for this record is for the second
                                       satellite in (3749) Balam system.


   3752 Camillo                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   3753 Cruithne                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3757 Anagolay                      
        Binzel 2019                    MITHNEOS Method: TAXON


   3761 Romanskaya                    
        Clark 2020                     Results table gives P = 9.456 h.


   3782 Celle                         
        Marchis 2012                   Hv found using assumged V-I = 0.88.


   3792 Preston                       
        Pravec 2016web                 The 23.8 h orbital period is based on a bimodal solution
                                       derived from a monomodal solution of 11.91 h. Possible, very
                                       shallow mutual events.

        Benishek 2017c                 If not binary, the two periods may indicate low-level
                                       tumbling.


   3800 Karayusuf                     
        Warner 2008m                   Two possible mutual events. Insufficient data to calculate a
                                       period.

        Binzel 2019                    MITHNEOS Method: VIS


   3833 Calingasta                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   3841 Dicicco                       
        Klinglesmith 2015d             Ds/Dp in Binary table is a minimum.


   3854 George                        
        Warner 2006f                   Suspicious attenutations but insufficient data for valid
                                       analysis.


   3858 Dorchester                    
        Binzel 2019                    MITHNEOS Method: VISNIR


   3908 Nyx                           
        Binzel 2019                    MITHNEOS Method: VISNIR


   3912 Troja                         
        Benishek 2021h                 Lightcurves availalbe at
                                       http://www.asu.cas.cz/~asteroid/03912_2021a_p1.png
                                       http://www.asu.cas.cz/~asteroid/03912_2021a_porb.png


   3920 Aubignan                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   3951 Zichichi                      
        Franco 2018c                   Some attenuations due to satellite observed. Period is based
                                       on single-period solution.


   3982 Kastel'                       
        Pravec 2005b                   Second period in binary table may be 2.918 h.


   3988 Huma                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4015 Wilson-Harrington             
        Also know as 107P/Wilson-Harrington. It has been observed to exhibit a cometary appearance.
        Photometry of this object may be contaminated by unresolved coma and not represent net
        nucleus brightness.

        Urakawa 2011                   The authors reported pole solutions. However, these are not
                                       considered reliable since they are based on data that are too
                                       limited for proper spin axis modeling.

        Urakawa 2012                   The authors provided four possible solutions that involved
                                       either tumbling, a binary object, or a single body in PA
                                       rotation. The spin axis and period are for for the PA
                                       solution.

        Binzel 2019                    MITHNEOS Method: eVISNIR 'Worked as' field is '1979 VA=165P'
                                       in original paper.


   4022 Nonna                         
        Behrend 2013web                Authors reported P = 1.31 h; this seems unlikely and so the
                                       double period was entered for the details record.


   4034 Vishnu                        
        Binzel 2019                    MITHNEOS Method: NIR


   4055 Magellan                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4142 Dersu-Uzala                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   4162 SAF                           
        Dose 2022b                     Author gave 3.850 h for a monomodal lightcurve. There are
                                       indications that a doubled-period, with bimodal lightcurve,
                                       might be preferred.


   4179 Toutatis                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4183 Cuno                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4197 Morpheus                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4205 David Hughes                  
        Binzel 2019                    MITHNEOS Method: VIS


   4225 Hobart                        
        Behrend 2023web                Reported as P = 8.3202 h. This gives either a 3 or 6 maximum
                                       lightcurve (depending on the impretation of the maximums).
                                       The period given is 2/3 the reported period with a bimodal
                                       lightcurve.


   4263 Abashiri                      
        Pravec 2012web                 A few deviations were see but nothing significant or
                                       convincing.


   4276 Clifford                      
        Binzel 2019                    MITHNEOS Method: VIS


   4336 Jasniewicz                    
        Owings 2018                    The longer period is determined from data and based on
                                       removing one night from the lightcurve.


   4337 Arecibo                       
        Gault 2022                     Second, confirming occulation on 2021 June 9. Dp = 24.4
                                       Ãƒâ€šÃ‚Â± 0.6 km, Ds = 13.0 Ãƒâ€šÃ‚Â± 1.5 (assuming circular
                                       shapes derived from occltation chords.


   4341 Poseidon                      
        Binzel 2019                    MITHNEOS Method: VIS


   4370 Dickens                       
        Benishek 2021j                 Secondary outside of events shows 0.04 mag lightcurve, a/b =
                                       1.3 Ã‚Â± 0.1.

        Pravec 2021web                 Tenative lightcurves at
                                       http://www.asu.cas.cz/~asteroid/04370_2021a_p1.png
                                       http://www.asu.cas.cz/~asteroid/04370_2021a_porb.png


   4401 Aditi                         
        Binzel 2019                    MITHNEOS Method: NIR


   4435 Holt                          
        Stephens 2018c                 Mutual events not tied to orbital period seen: possible
                                       second satellite.

        Stephens 2018g                 Attenuations not tied to the orbital period may indicate a
                                       second satellite. See original paper for the evolution of the
                                       primary lightcurve and mutual events.

        Binzel 2019                    MITHNEOS Method: VIS


   4450 Pan                           
        Carbognani 2008b               Values for G and Pv were assumed based on Wisniewski (1997).

        Binzel 2019                    MITHNEOS Method: NIR


   4451 Grieve                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   4486 Mithra                        
        The amplitude, A = 0.5, is an estimate based on the derived shape of the asteroid and an
        equatorial view.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4492 Debussy                       
        Marchis 2012                   Hv found using V-R 0.54.


   4495 Dassanowsky                   
        Ambiguity is for P1. Binary status not in doubt.

        Warner 2019i                   Ambiguity is for P1. Adopted period is favored because of
                                       estimated size ratio of system and binary modeling (Pravec et
                                       al., 2010)


   4503 Cleobulus                     
        Binzel 2019                    MITHNEOS Method: VIS


   4524 Barklajdetolli                
        Athanasopoulos 2022            The original paper reported Beta2 = 93 deg. Values |beta| >
                                       90 are not allowed in the LCDB and so B2 = 90 was used.


   4528 Berg                          
        Fornas 2023a                   Polakis data (ALCDEF, 2018 Feb) included in solution.


   4541 Mizuno                        
        Pray 2015b                     Ds/Dp >= 0.24


   4544 Xanthus                       
        Binzel 2019                    MITHNEOS Method: NIR


   4555 Josefaperez                   
        Pravec 2007web                 Variations in mean levels of the calibrated Ondrejov R data
                                       suggest that there may be a rotation of an unresolved
                                       satellite.


   4558 Janesick                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   4587 Rees                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4660 Nereus                        
        The pV = 0.3 is based on Pravec et al. (2021web) assumption of G = 0.43. Using the default
        pV = 0.2 gives a diameter of 0.516 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4666 Dietz                         
        Pravec 2015web                 One suspected event captured.

        Oey 2018a                      Data from 2011 and 2015 included in analysis. Possible third
                                       period seen in 2015 and 2018 data.

        Warner 2021g                   Alternate orbital solution is 33.4 h, which is near that
                                       found in 2018 and for which the mutual events were much
                                       better defined.


   4688 1980 WF                       
        This note applies to all Binzel 2019 (2019Icar..324...41B) detail records:  VIS indicates
        visible data only.  NIR indicates near-infrared data only.  VISNIR indicates both. eVISNIR
        indicates the visible portion of the spectrum is from the Eight-Color Asteroid Survey (ECAS,
        Zellner et al. 1985) sVis indicates the visible portion of the spectrum is from the Sloan
        Digital Sky Survey (SDSS, Ivezic et al. 2001). TAXON indicates the type is reported in the
        literature; see the source listed in the 'Taxon' reference column of the original file.  For
        visible data only (VIS), the taxonomic type is from the Bus classification system (Bus and
        Binzel 2002). For visible plus near-infrared data (VISNIR), the taxonomic type is from the
        Bus-DeMeo classification system (DeMeo et al. 2009).  '-comp' refers to the broad taxonomic
        complex. When multiple taxonomic classes are listed, they are in subjective order of most
        likely type first. ':' indicates the assignment is uncertain.

        Binzel 2019                    MITHNEOS Method: VISNIR


   4690 Strasbourg                    
        Warner 2011j                   Multiple solutions possible because of the limited data set.
                                       Analysis by Petr Pravec.


   4708 Polydoros                     
        Stephens 2018i                 Period taken from plot. Results table and text each have a
                                       different period.


   4718 Araki                         
        Pravec 2017web                 The nature of the two periods is uncertain. They could be the
                                       result of a binary or low level tumbling, thus this record
                                       carries both flags.


   4729 Mikhailmil'                   
        Ruthroff 2012a                 Lightcurve has very unusual shape. The period could really
                                       lie between 15-30 h.


   4765 Wasserburg                    
        Pravec 2019b                   Paired with (350716) 2001 XO105.


   4775 Hansen                        
        Binzel 2019                    MITHNEOS Method: sVISNIR


   4788 Simpson                       
        Sogorb 2021                    Third period (3.1506 h) may be due to eclipsing/occultating
                                       secondary or a third body.


   4905 Hiromi                        
        Pravec 2019b                   Paired with (7813) Anderserikson.


   4910 Kawasato                      
        Binzel 2019                    MITHNEOS Method: VIS


   4947 Ninkasi                       
        Binzel 2019                    MITHNEOS Method: VIS


   4953 1990 MU                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   4954 Eric                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   4957 Brucemurray                   
        Binzel 2019                    MITHNEOS Method: VIS


   4995 Griffin                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5003 Silvanominuto                 
        Waszczak (2016) H values are based on G12 system. The G12 value is given instead of G and
        carries 'G' for the source flag. The G2 value is NULL. The LCDB U value is based on the
        Waszczak et al. 'relflag' value, with relflag = 0 given U = 1 and relflag = 1 given U = 2


   5011 Ptah                          
        Binzel 2019                    MITHNEOS Method: VISNIR


   5026 Martes                        
        Pravec 2019b                   Paired with 2005 WW113.


   5066 Garradd                       
        Binzel 2019                    MITHNEOS Method: sVIS


   5076 Lebedev-Kumach                
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5104 Skripnichenko                 
        Behrend 2023web                Reported as 5.56457 h. The amplitude and high degree of
                                       symmentry of the quadramodal lightcurve make this unlikely.


   5131 1990 BG                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5143 Heracles                      
        Taylor 2012b                   Dp = 3.6 ± 1.2 km; Ds = 0.6 ± 0.3 km. Orbital period of 16 h
                                       is based on period 14-17 h. A period of 40-57 h cannot be
                                       excluded, but it is inconsistent with the assumption of a
                                       synchronously rotating secondary.

        Binzel 2019                    MITHNEOS Method: VISNIR


   5145 Pholus                        
        Tegler 2005                    Dimensions (diameters) determined by calculation to be 310 X
                                       160 x 150 km. This gives an effective spheroidal diameter of
                                       ~190 km.

        Belskaya 2010b                 To derive H, used V-R=0.77 and phase coefficient (not G) of
                                       0.083 mag/degree.


   5230 Asahina                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5247 Krylov                        
        Lee 2020                       P = 82.28 is the strongest apparent period, the conjunction
                                       of the period of rotation (368.7 h) and rotation (67.27 h).


   5261 Eureka                        
        Binzel 2019                    MITHNEOS Method: VISNIR

        Skiff 2019b                    Raw plot shows total eclipse/occultation due to satellite.

        Skiff 2019b                    Raw plot shows mutual event due to satellite.


   5275 Zdislava                      
        Binzel 2019                    MITHNEOS Method: VIS


   5332 Davidaguilar                  
        Binzel 2019                    MITHNEOS Method: NIR


   5349 Paulharris                    
        Binzel 2019                    MITHNEOS Method: VIS


   5381 Sekhmet                       
        Binzel 2019                    MITHNEOS Method: NIR


   5384 Changjiangcun                 
        The low WISE and AKARI albedos indicate that C-type is a better choice rather than the LCDB
        default of ES for Hungaria members.


   5392 Parker                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   5402 Kejosmith                     
        Benishek 2018j                 The ambiguity is for Porb. It may be 32.62 h instead of the
                                       adopted 16.31 h.


   5407 1992 AX                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5425 Vojtech                       
        Vander Haagen 2012a            Author reported a trimodal solution of 3.972 h. This is
                                       considered highly unlikely.


   5496 1973 NA                       
        Binzel 2019                    MITHNEOS Method: NIR


   5510 1988 RF7                      
        Binzel 2019                    MITHNEOS Method: VIS


   5535 Annefrank                     
        Hillier 2011                   Stardust and ground-based observations.


   5573 Hilarydownes                  
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5585 Parks                         
        Binzel 2019                    MITHNEOS Method: VIS


   5587 1990 SB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5604 1992 FE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5620 Jasonwheeler                  
        Binzel 2019                    MITHNEOS Method: NIR


   5626 Melissabrucker                
        Binzel 2019                    MITHNEOS Method: VISNIR


   5642 Bobbywilliams                 
        Binzel 2019                    MITHNEOS Method: NIR


   5645 1990 SP                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5646 1990 TR                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5649 Donnashirley                  
        Binzel 2019                    MITHNEOS Method: VIS


   5653 Camarillo                     
        Binzel 2019                    MITHNEOS Method: NIR


   5656 Oldfield                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   5660 1974 MA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5674 Wolff                         
        Aznar 2016b                    Ds/Dp >= 0.80


   5693 1993 EA                       
        Binzel 2019                    MITHNEOS Method: eVISNIR


   5720 Halweaver                     
        Binzel 2019                    MITHNEOS Method: NIR


   5732 1988 WC                       
        Binzel 2019                    MITHNEOS Method: VIS


   5751 Zao                           
        Binzel 2019                    MITHNEOS Method: VIS


   5786 Talos                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   5797 Bivoj                         
        Binzel 2019                    MITHNEOS Method: TAXON


   5817 Robertfrazer                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   5828 1991 AM                       
        Binzel 2019                    MITHNEOS Method: VIS


   5836 1993 MF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   5867 1988 RE                       
        Binzel 2019                    MITHNEOS Method: NIR


   5870 Baltimore                     
        Binzel 2019                    MITHNEOS Method: VIS


   5899 Jedicke                       
        Warner 2010h                   The amplitude of the primary was too low to establish a
                                       period with certainty. The mutual events, however, were
                                       well-defined.

        Warner 2010n                   The amplitude of the primary was too low to establish a
                                       period with certainty. The mutual events, however, were
                                       well-defined.


   5968 Trauger                       
        Warner 2014d                   Unexplained 'event' on Sep 5. Possible period solutions
                                       assuming a satellite are P_orb = 15.9 or 31.7 h.


   6037 1988 EG                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6041 Juterkilian                   
        Binzel 2019                    MITHNEOS Method: sVIS


   6042 Cheshirecat                   
        Binzel 2019                    MITHNEOS Method: sVIS


   6047 1991 TB1                      
        Binzel 2019                    MITHNEOS Method: VIS


   6053 1993 BW3                      
        Warner 2015s                   Result of combining data sets from 2015 January and March.

        Binzel 2019                    MITHNEOS Method: TAXON


   6063 Jason                         
        Warner 2017n                   Radar could not confirm long period.

        Binzel 2019                    MITHNEOS Method: NIR


   6070 Rheinland                     
        Vokrouhlicky 2011              H_R actually found. Authors used V-R = 0.49 ± 0.05 to convert
                                       to H.

        Vokrouhlicky 2017b             See paper for discussion of pole solution uncertainties.

        Pravec 2019b                   Paired with (54827) Kurpfalz.


   6084 Bascom                        
        Pravec 2012a                   Residual variations of 0.02 mag may indicate rotation of a
                                       satellite.


   6170 Levasseur                     
        Binzel 2019                    MITHNEOS Method: sVIS


   6178 1986 DA                       
        Binzel 2019                    MITHNEOS Method: NIR


   6183 Viscome                       
        Binzel 2019                    MITHNEOS Method: sVIS


   6186 Zenon                         
        Benishek 2017b                 S1 has amplitude of 0.04 mag.


   6239 Minos                         
        Binzel 2019                    MITHNEOS Method: VISNIR


   6261 Chione                        
        Binzel 2019                    MITHNEOS Method: sVIS


   6369 1983 UC                       
        Pravec 2019b                   Paired with (510132) 2010 UY57. The Observing Circumstances
                                       are for lightcurves from 2013.


   6386 Keithnoll                     
        Binzel 2019                    MITHNEOS Method: VISNIR


   6411 Tamaga                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   6444 Ryuzin                        
        Binzel 2019                    MITHNEOS Method: sVIS


   6455 1992 HE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6456 Golombek                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a p_V = 0.18.

        Binzel 2019                    MITHNEOS Method: VISNIR


   6489 Golevka                       
        Binzel 2019                    MITHNEOS Method: TAXON


   6500 Kodaira                       
        Binzel 2019                    MITHNEOS Method: VIS


   6523 Clube                         
        Binzel 2019                    MITHNEOS Method: sVIS


   6569 Ondaatje                      
        Binzel 2019                    MITHNEOS Method: VIS


   6585 O'Keefe                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   6611 1993 VW                       
        Pravec 2005web                 The second period maybe the secondary's rotation or the
                                       orbtial period.

        Binzel 2019                    MITHNEOS Method: VISNIR


   6764 Kirillavrov                   
        Polakis 2022a                  Analysis of TESS data (Pal et al, 2020, Ap. J. 247, A26).


   6809 Sakuma                        
        Pravec 2018web                 Suspected mutual events observed on two nights.


   6847 Kunz-Hallstein                
        Binzel 2019                    MITHNEOS Method: VIS


   6909 Levison                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7002 Bronshten                     
        Binzel 2019                    MITHNEOS Method: VIS


   7025 1993 QA                       
        Binzel 2019                    MITHNEOS Method: sVIS


   7079 Baghdad                       
        Binzel 2019                    MITHNEOS Method: sVIS


   7088 Ishtar                        
        Binzel 2019                    MITHNEOS Method: VIS


   7092 Cadmus                        
        Binzel 2019                    MITHNEOS Method: NIR


   7132 Casulli                       
        Franco 2020e                   The original gives Ds/Dp ~ 0.21. The 0.11 mag attenuation
                                       gives Ds/Dp ~ 0.33. The latter is used in the lc_binaries
                                       table.


   7165 Pendleton                     
        Behrend 2023web                Data show possible binary events.


   7187 Isobe                         
        Warner 2011o                   Weak secondary period: P = 16.33 ± 0.04 h, A = 0.12 ± 0.01
                                       mag.

        Warner 2011o                   Weak secondary period: P = 16.378 ± 0.05 h, A = 0.05 ± 0.01
                                       mag.


   7304 Namiki                        
        Binzel 2019                    MITHNEOS Method: VISNIR


   7307 Takei                         
        Benishek 2021e                 Secondary has lightcurve amplitude (in the combined primary
                                       plus secondary lightcurve) of 0.05 mag.


   7335 1989 JA                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


   7336 Saunders                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   7341 1991 VK                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7343 Ockeghem                      
        Pravec 2019b                   Paired with (154634) 2003 XX38.


   7350 1993 VA                       
        Binzel 2019                    MITHNEOS Method: NIR


   7358 Oze                           
        Binzel 2019                    MITHNEOS Method: VISNIR


   7393 Luginbuhl                     
        Warner 2019k                   Out of event satellite lightcurve indicates elongation of
                                       about 1.7:1


   7474 1992 TC                       
        Binzel 2019                    MITHNEOS Method: VIS


   7480 Norwan                        
        Binzel 2019                    MITHNEOS Method: VIS


   7482 1994 PC1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   7488 Robertpaul                    
        Stephens 2022e                 P2 isn't a formal solution, just that one that, when
                                       subtracted, results in a U = 3- P1.


   7517 Alisondoane                   
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   7560 Spudis                        
        Warner 2013d                   There is a weak secondary period of 22.6 h. The 2004
                                       apparition showed a possible binary with orbital period of
                                       23.4 h.


   7604 Kridsadaporn                  
        Binzel 2019                    MITHNEOS Method: VIS


   7722 Firneis                       
        This applies to all Colazo 2021d entries. There are up to three details entries per object:
        1) H-G using Gaia GR magnitudes, 2) H-G with GR magnitudes transformed to V and adding
        ground-based data to include phase angles < 10 deg, and 3) H-G1,G2 using the same magnitudes
        as in 2. Only results where there were valid numbers for H and HErr and the G or G1/G2
        errors were <= 1.0 were included in the LCDB entries. H/HErr were rounded to two decimal
        places and G/GErr values were rounded to three decimal places. For a new summary record, the
        MPCOrb values are used for H and G for groups 1 and 3. This provides the necessary
        consitency for H when generating frequency-diameter plots from LCDB data, which have have
        been historically based on the H(V)-G system. For the Details record, the H Band is 'GR' for
        group 1 and 'V' for groups 2 and 3. To help convey that the V magnitudes were derived from
        GR and assumed V-R magnitudes, the H Method is 'D' (Derived). The G Method will be empty for
        groups 1 and 2 since, regardless


   7753 1988 XB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7757 Kameya                        
        Warner 2011web                 Data too noisy to give reasonable period or amplitude.


   7758 Poulanderson                  
        Warner 2012m                   Only one event well seen, maybe a second. Several other
                                       orbital period solutions fit, ranging out to about 100 hours.
                                       


   7760 1990 RW3                      
        Galad 2010c                    Combined with data from Pray (2006f)


   7813 Anderserikson                 
        Pravec 2019b                   Paired with (4905) Hiromi.


   7818 Muirhead                      
        Binzel 2019                    MITHNEOS Method: sVIS


   7822 1991 CS                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7888 1993 UC                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7889 1994 LX                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   7977 1977 QQ5                      
        Binzel 2019                    MITHNEOS Method: TAXON


   8013 Gordonmoore                   
        Binzel 2019                    MITHNEOS Method: VISNIR


   8014 1990 MF                       
        Binzel 2019                    MITHNEOS Method: NIR


   8034 Akka                          
        Binzel 2019                    MITHNEOS Method: TAXON


   8037 1993 HO1                      
        Binzel 2019                    MITHNEOS Method: VIS


   8167 Ishii                         
        Pravec 2021web                 Two attenutions suspected on Feb 6 and 9.


   8176 1991 WA                       
        Binzel 2019                    MITHNEOS Method: TAXON


   8201 1994 AH2                      
        Binzel 2019                    MITHNEOS Method: TAXON


   8306 Shoko                         
        Polishook 2014a                Likely mutual events seen twice, but insufficient data to
                                       determine the orbital period for a satellite.

        Pravec 2014a                   Possible third body.

        Pravec 2019b                   Paired with 2011 SR158.


   8345 Ulmerspatz                    
        The lightcurves from the 2011-2012 apparition give strong indications that this asteroid
        might be a tidally-locked binary of nearly equal sized components, similar to 90 Antiope.

        Klinglesmith 2012c             When using the full data set, P = 17.1192 ± 0.0008 h.


   8355 Masuo                         
        Binzel 2019                    MITHNEOS Method: sVIS


   8356 Wadhwa                        
        Pravec 2008web                 http://www.asu.cas.cz:80/~asteroid/08356.png


   8369 Miyata                        
        Warner 2011s                   Subtracting a weak secondary period of 49.24 h improves the
                                       RMS fit of the 2.73 h period noticeably.


   8373 Stephengould                  
        Binzel 2019                    MITHNEOS Method: VISNIR


   8444 Popovich                      
        Binzel 2019                    MITHNEOS Method: sVIS


   8566 1996 EN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


   8567 1996 HW1                      
        Magri 2011                     Authors give ellipsoid of 3.8x1.6x1.5 km, which gives an
                                       effective spheroidal diameter of about 2 km.  Composite
                                       lightcurves were not provided, only overlays of the
                                       lightcurve data over the model curve. The U=3 rating refers
                                       to the overall quality of the data set used to find the pole,
                                       shape, and sidereal period.

        Trilling 2016                  This applies to all Trilling 2016 (AJ 152): the listed errors
                                       for the diameter and albedo are the larger of the ± values,
                                       which were not the same.

        Binzel 2019                    MITHNEOS Method: VISNIR


   8651 Alineraynal                   
        Binzel 2019                    MITHNEOS Method: VIS


   8828 1988 RC7                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


   8861 Jenskandler                   
        Hayes-Gehrke 2023c             P = 4.500 is a trimodal solution.


   8864 1991 VU                       
        The albedo error given for Masiero 2017 is the maximum possible value when converting from
        albedo values from log space to value space.


   9068 1993 OD                       
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2019b                   Paired with (455327) 2002 OP28.

        Pravec 2019b                   Paired with (455327) 2002 OP28.


   9069 Hovland                       
        Marchis 2012                   Hv assumed V-R = 0.54.


   9082 Leonardmartin                 
        Binzel 2019                    MITHNEOS Method: VIS


   9162 Kwiila                        
        Binzel 2019                    MITHNEOS Method: TAXON


   9202 1993 PB                       
        Binzel 2019                    MITHNEOS Method: sVIS


   9400 1994 TW1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


   9671 Hemera                        
        Binzel 2019                    MITHNEOS Method: sVIS


   9783 Tensho-kan                    
        Pravec 2019b                   Paired with (348018) 2003 SF334.


   9856 1991 EE                       
        Binzel 2019                    MITHNEOS Method: TAXON


   9881 Sampson                       
        Binzel 2019                    MITHNEOS Method: sVIS


   9950 ESA                           
        Binzel 2019                    MITHNEOS Method: NIR


   9969 Braille                       
        Binzel 2019                    MITHNEOS Method: VIS


   9992 1997 TG19                     
        Higgins 2006f                  Incorrectly referenced in text as 1997 TH19.

        Binzel 2019                    MITHNEOS Method: NIR


  10051 Albee                         
        Binzel 2019                    MITHNEOS Method: sVIS


  10115 1992 SK                       
        Binzel 2019                    MITHNEOS Method: sVISNIR

        Durech 2022                    YORP Parameter: 8.3(6) * (10^8 rad d^-2)


  10123 Fideoja                       
        Pravec 2019b                   Paired with (117306) 2004 VF21.


  10132 Lummelunda                    
        Benishek 2018f                 See original paper for evolution of the primary lightcurve
                                       and attenuation events.

        Salvaggio 2018b                Shorter period in ambiguous table comes from lightcurve plot
                                       while longer period in detail record comes from text.


  10145 1994 CK1                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  10150 1994 PN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  10165 1995 BL2                      
        Binzel 2019                    MITHNEOS Method: VIS


  10199 Chariklo                      
        Belskaya 2010b                 To derive H, used V-R=0.48 and phase coefficient (not G) of
                                       0.06 mag/degree.


  10247 Amphiaraos                    
        McNeill 2021                   This note applies to all entries for McNeill et al. (2021;
                                       Plan. Sci. J. 2, A6). The H-G (Bowell) model was used for
                                       finidng Hc/Ho and, from all appearances, Go not Gv. Table 1
                                       lists Hv values taken from the JPL database and not Ho (the
                                       orange data being far more prevalent) or Hc. The error for Hv
                                       was presumed to be 0.05 mag


  10261 Nikdollezhal'                 
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  10295 Hippolyta                     
        Binzel 2019                    MITHNEOS Method: NIR


  10296 Rominadisisto                 
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  10302 1989 ML                       
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2022i                   Final solution when using additive period anlaysis required
                                       P3 = 18.90, A3=0.15.


  10502 Armaghobs                     
        Binzel 2019                    MITHNEOS Method: sVIS


  10563 Izhdubar                      
        Binzel 2019                    MITHNEOS Method: TAXON


  10779 1991 LW                       
        Warner 2011o                   One-night stand. Period is based on a half-period analysis.


  11001 Andrewulff                    
        Pravec 2012web                 Partial attenuations seen but not enough to confirm binary
                                       status.


  11054 1991 FA                       
        Binzel 2019                    MITHNEOS Method: NIR


  11066 Sigurd                        
        Binzel 2019                    MITHNEOS Method: VISNIR


  11284 Belenus                       
        Binzel 2019                    MITHNEOS Method: NIR


  11286 1990 RO8                      
        Pravec 2019b                   Paired with (59394) 1999 FZ23.


  11311 Peleus                        
        Binzel 2019                    MITHNEOS Method: VIS


  11351 Leucus                        
        Mottola 2020                   V-SR: 0.313 Ãƒâ€šÃ‚Â± 0.021


  11398 1998 YP11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  11405 1999 CV3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  11500 Tomaiyowit                    
        Binzel 2019                    MITHNEOS Method: VIS


  11677 1998 DY4                      
        Pravec 2019b                   Paired with (412065) 2013 ET86.

        Pravec 2019b                   Paired with (412065) 2013 ET86.


  11836 Eileen                        
        Binzel 2019                    MITHNEOS Method: sVIS


  11842 Kap'bos                       
        Ye 2011                        Asteroid pair with (228747) 2002 VH3, for which Ye found B-V
                                       = 0.704 ± 0.154, V-R = 0.480 ± 0.057, and V-I = 0.829 ±
                                       0.111.


  11885 Summanus                      
        Binzel 2019                    MITHNEOS Method: NIR


  12016 Green                         
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  12326 Shirasaki                     
        Pray 2017a                     Secondary period may be due to rotation of the satellite or a
                                       third body. If the former, the system would be
                                       fully-asynchronous and not singly-asychronous.


  12376 Cochabamba                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  12538 1998 OH                       
        Vaduvescu 2017                 Sloan g magnitudes

        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2019h                   Two close solutions that are not harmonically related. See
                                       the binaries file. The two periods could also be the result
                                       of tumbling. Both possibilties fit the data.

        Warner 2019p                   The split-halves plot for 5.16 h essentially duplicates the
                                       two halves. In this case, the shorter period was adopted.


  12711 Tukmit                        
        Binzel 2019                    MITHNEOS Method: VISNIR


  12923 Zephyr                        
        Binzel 2019                    MITHNEOS Method: NIR


  13123 Tyson                         
        Pravec 2022web                 No lightcurve for suspected secondary period.


  13186 1996 UM                       
        Wang 2021                      Sideral period for (38, +35): 4.29828 h


  13284 1998 QB52                     
        Pravec 2019b                   Paired with (154828) 2004 RT8.

        Pravec 2019b                   Paired with (154828) 2004 RT8.


  13331 1998 SU52                     
        Warner 2011k                   A weak secondary period of ~15.1 h was observed but could not
                                       be explained.


  13355 1998 TP17                     
        Pravec 2023web                 Second period is well-established. It could be due to
                                       tumbling or a satellite, therefore, the asteroid is listed as
                                       both types.


  13553 Masaakikoyama                 
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2019b                   Single period found 39 h, very similar to Pravec et al. 2005.


  13651 1997 BR                       
        Binzel 2019                    MITHNEOS Method: TAXON


  13732 Woodall                       
        Ye 2011                        Asteroid pair with (1979) Sakharov, for which Ye found B-V =
                                       1.086 and V-R = 0.409.


  13819 1999 SX5                      
        Binzel 2019                    MITHNEOS Method: sVIS


  14017 1994 NS                       
        Binzel 2019                    MITHNEOS Method: sVIS


  14222 1999 WS1                      
        Binzel 2019                    MITHNEOS Method: NIR


  14309 Defoy                         
        Binzel 2019                    MITHNEOS Method: sVIS


  14395 Tommorgan                     
        Warner 2013d                   Second period of 40.4 provided by P. Pravec. The second
                                       solution is not unique. Others are possible.


  14402 1991 DB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  14581 1998 RT4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  14806 1981 EV25                     
        Pravec 2019b                   Paired with (496028) 2008 SC9.


  14827 Hypnos                        
        Binzel 2019                    MITHNEOS Method: TAXON


  14868 1990 RA7                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  14875 1990 WZ1                      
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


  14923 1994 TU3                      
        Warner 2009b                   Recalibration of comp star mags led to different period.


  14982 1997 TH19                     
        Binzel 2019                    MITHNEOS Method: sVIS


  15107 Toepperwein                   
        Pravec 2019b                   Paired with (291188) 2006 AL54.

        Pravec 2021b                   Asteroid pair with (291188) 2006 AL54.


  15350 Naganuma                      
        Pravec 2010web                 Period taken from 2005 observations.


  15430 1998 UR31                     
        Pravec 2010web                 Brightness drops by >0.10 mag seen on 2010-05-06 and 07, but
                                       period not established.


  15607 2000 GA124                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  15609 Kosmaczewski                  
        Binzel 2019                    MITHNEOS Method: sVIS


  15700 1987 QD                       
        Durkee 2010c                   Two possible periods for the orbit were 50.3 and 62.9 h.
                                       Neither could be conclusively established.

        Binzel 2019                    MITHNEOS Method: sVIS


  15745 Yuliya                        
        Warner 2018m                   The primary and orbital period were found by forcing the data
                                       to fit near the periods found by Aznar et al. (2018). The
                                       listed primary period is one of dozens of possible solutions.
                                       

        Binzel 2019                    MITHNEOS Method: VISNIR


  15778 1993 NH                       
        Warner 2015e                   Possible wide binary. The long period is the rotation of the
                                       primary.


  15817 Lucianotesi                   
        Binzel 2019                    MITHNEOS Method: VIS


  15822 Genefahnestock                
        Warner 2011c                   Suspected events seen on three nights in 2010 mid-June. None
                                       seen in 2010 late June or early July.


  16064 Davidharvey                   
        Binzel 2019                    MITHNEOS Method: VIS


  16126 1999 XQ86                     
        Pravec 2019b                   Paired with 2015 AH1.


  16142 Leung                         
        Binzel 2019                    MITHNEOS Method: sVIS


  16426 1988 EC                       
        Diameter and albedo based on H from Warner (2012) and application of Harris and Harris
        (1997) correction to WISE diameter and albedo.


  16635 1993 QO                       
        Binzel 2019                    MITHNEOS Method: sVIS


  16636 1993 QP                       
        Binzel 2019                    MITHNEOS Method: NIR


  16657 1993 UB                       
        Binzel 2019                    MITHNEOS Method: VIS


  16815 1997 UA9                      
        Pravec 2019b                   Paired with (436551) 2011 GD83.


  16816 1997 UF9                      
        Binzel 2019                    MITHNEOS Method: sVIS


  16834 1997 WU22                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  16868 1998 AK8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  16960 1998 QS52                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  17188 1999 WC2                      
        Binzel 2019                    MITHNEOS Method: NIR


  17198 Gorjup                        
        Pravec 2019b                   Paired with (229056) 2004 FC126.


  17274 2000 LC16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  17288 2000 NZ10                     
        Pravec 2019b                   Paired with (203489) 2002 AL80.


  17435 di Giovanni                   
        Binzel 2019                    MITHNEOS Method: sVIS


  17511 1992 QN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  17700 Oleksiygolubov                
        Pray 2018a                     Additional attenuations of 0.14-0.18 mag are not tied to
                                       orbital period and may indicate a third body.


  18106 Blume                         
        Binzel 2019                    MITHNEOS Method: NIR


  18109 2000 NG11                     
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  18172 2000 QL7                      
        Binzel 2019                    MITHNEOS Method: NIR


  18181 2000 QD34                     
        Binzel 2019                    MITHNEOS Method: sVIS


  18514 1996 TE11                     
        Binzel 2019                    MITHNEOS Method: VIS


  18620 1998 DS10                     
        Binzel 2019                    MITHNEOS Method: NIR


  18736 1998 NU                       
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2019m                   Despite the low amplitude of the secondary period, the period
                                       spectrum clearly favors 11.95 h or 23.9 h. The low amplitude
                                       and nearly Earth day period of the secondary lightcurve make
                                       a weak case for being binary.


  18882 1999 YN4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  18916 2000 OG44                     
        Binzel 2019                    MITHNEOS Method: NIR


  19127 Olegefremov                   
        Binzel 2019                    MITHNEOS Method: VISNIR


  19204 Joshuatree                    
        Stephens 2016h                 Main period forced to solution from 2016 data.


  19261 1995 MB                       
        Behrend 2021web                Period was reported by Behrend as 9.130 h. However, that
                                       solution is based on only two nights and at significant phase
                                       angle, ~19 deg, while the 2010 curves from Cabognani and
                                       Owings are at a considerably lower phase angle, 5-6 deg. The
                                       latter, along with fairly large amplitude, would make a
                                       double period, quad extrema, curve very unlikely, bordering
                                       on impossible. On the other hand, the Behrend curve could be
                                       essentially monomodal, with just a very muted secondary
                                       maximum. Also troubling is the very sharp maxima of the
                                       Behrend fit. Sharp minima are expected and can be even more
                                       extreme due to shadowing, but very narrow maxima (broadside
                                       view) are much less expected.


  19289 1996 HY12                     
        Pravec 2019b                   Paired with (278067) 2006 YY40.


  19309 1996 UK1                      
        Galad 2008c                    Several bimodal solutions possible in the range of 4.16-5.91
                                       h.


  19356 1997 GH3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  19388 1998 DQ3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  19764 2000 NF5                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021a                   P3/A3 11.931 h/0.08 mag produces much cleaner P1/P2
                                       lightcurves. It doesn't have a physical nature but filters
                                       the effects of near-Earth day commensurate observations.


  20062 1993 QB3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  20086 1994 LW                       
        Binzel 2019                    MITHNEOS Method: NIR


  20236 1998 BZ7                      
        Binzel 2019                    MITHNEOS Method: TAXON


  20255 1998 FX2                      
        Binzel 2019                    MITHNEOS Method: TAXON


  20384 1998 KW51                     
        Clark 2021                     4 uneven maximums for given period.


  20425 1998 VD35                     
        Binzel 2019                    MITHNEOS Method: VIS


  20429 1998 YN1                      
        Binzel 2019                    MITHNEOS Method: NIR


  20446 1999 JB80                     
        Binzel 2019                    MITHNEOS Method: sVIS


  20452 1999 KG4                      
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  20691 1999 VY72                     
        Binzel 2019                    MITHNEOS Method: sVIS


  20749 2000 AD199                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  20790 2000 SE45                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  20826 2000 UV13                     
        Binzel 2019                    MITHNEOS Method: VIS


  20882 Paulsanchez                   
        Warner 2019n                   Data split into two sets to show evolution of the mutual
                                       events.


  20958 A900 MA                       
        Binzel 2019                    MITHNEOS Method: sVIS


  21028 1989 TO                       
        Pravec 2019b                   Paired with (481085) 2005 SA135.


  21088 Chelyabinsk                   
        Binzel 2019                    MITHNEOS Method: VISNIR


  21149 Kenmitchell                   
        Warner 2024                    2015 Results: A third period, P3 = 60.4 ± 0.1 h, A3 = 0.16 ±
                                       0.02 mag, was required to get P1/P2 similar to 2023.


  21436 Chaoyichi                     
        Pravec 2019b                   Paired with (334916) 2003 YK39.


  21601 1998 XO89                     
        French 2013                    Authors confirmed that the period in paper's table and not
                                       the one in the lightcurve plot is the correct value.


  21709 Sethmurray                    
        Yeh 2020                       For Yeh 2020, the amplitude error was found with max(0.01,
                                       0.1*YehAmp)


  21966 Hamadori                      
        Binzel 2019                    MITHNEOS Method: sVIS


  22099 2000 EX106                    
        Binzel 2019                    MITHNEOS Method: VIS


  22449 Ottijeff                      
        Binzel 2019                    MITHNEOS Method: VIS


  22753 1998 WT                       
        Binzel 2019                    MITHNEOS Method: eVISNIR


  22771 1999 CU3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  22807 1999 RK7                      
        Binzel 2019                    MITHNEOS Method: sVIS


  22891 1999 SO11                     
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


  23183 2000 OY21                     
        Binzel 2019                    MITHNEOS Method: NIR


  23186 2000 PO8                      
        Warner 2021i                   Model dimensions (c = 1): a/b = 1.2, a/c = 2.3.


  23187 2000 PN9                      
        Binzel 2019                    MITHNEOS Method: NIR


  23548 1994 EF2                      
        Binzel 2019                    MITHNEOS Method: VIS


  23615 1996 FK12                     
        Warner 2015l                   A suspected 'wide binary'. The long period is the primary.
                                       The short period (U = 3) is for the fully asynchronous
                                       satellite.


  23621 1996 PA                       
        Binzel 2019                    MITHNEOS Method: sVIS


  23692 Nandatianwenners              
        Clark 2020                     Result of combining data from 2015 and 2019. The DateObs is
                                       the mid-date for the 2015 data set.

        Clark 2020                     Results table gives P = 9.315 h.


  23714 1998 EC3                      
        Binzel 2019                    MITHNEOS Method: TAXON


  23971 1998 YU9                      
        The Masi et al. paper gave this as a C-type on the basis of a netural spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  23983 1999 NS11                     
        Binzel 2019                    MITHNEOS Method: sVIS


  23998 1999 RP29                     
        Pravec 2019b                   Paired with (205383) 2001 BV47.


  24077 1999 TD233                    
        Warner 2014f                   Given periods may not be actual values, but linear
                                       combinations of the true NPAR periods.


  24445 2000 PM8                      
        Monteiro 2018b                 For all Monteiro 2018b: if the table date, period, and/or
                                       amplitude disagreed with the lightcurve, the value(s) in the
                                       plot were used.

        Binzel 2019                    MITHNEOS Method: VISNIR


  24475 2000 VN2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  24693 1990 SB2                      
        Binzel 2019                    MITHNEOS Method: sVIS


  24761 Ahau                          
        Binzel 2019                    MITHNEOS Method: sVISNIR


  24814 1994 VW1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  25021 Nischaykumar                  
        Pravec 2019b                   Paired with (453818) 2011 SJ109.


  25037 1998 QC37                     
        Binzel 2019                    MITHNEOS Method: sVIS


  25143 Itokawa                       
        Mueller 2011a                  H and G taken from other sources.

        Nishihara 2018                 Using all data from 2001-2004, P = 12.1324 h

        Binzel 2019                    MITHNEOS Method: VISNIR


  25330 1999 KV4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  25332 1999 KK6                      
        Warner 2013b                   Alternate suspected P2: 16.18 h.


  25362 1999 TH24                     
        Binzel 2019                    MITHNEOS Method: sVIS


  25884 Asai                          
        Pravec 2019b                   Paired with (48527) 1993 LC1.


  25916 2001 CP44                     
        Warner 2018m                   Period revised based on 2018 data/analysis.

        Binzel 2019                    MITHNEOS Method: VISNIR


  26093 1987 UA1                      
        Pravec 2012web                 Double period not formally excluded.


  26166 1995 QN3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  26209 1997 RD1                      
        Binzel 2019                    MITHNEOS Method: VIS


  26308 1998 SM165                    
        Brown 2002                     Sep ~ 6000 km


  26416 1999 XM84                     
        Pravec 2019b                   Paired with (214954) 2007 WO58.


  26420 1999 XL103                    
        Pravec 2019b                   Paired with 2012 TS209.


  26737 Adambradley                   
        Stephens 2020c                 Weak secondary period of 20-40 h noticeably improved the RMS
                                       for the 2.7 h solution.


  26760 2001 KP41                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  26858 Misterrogers                  
        Binzel 2019                    MITHNEOS Method: NIR


  26879 Haines                        
        Binzel 2019                    MITHNEOS Method: VIS


  27002 1998 DV9                      
        Binzel 2019                    MITHNEOS Method: TAXON


  27346 2000 DN8                      
        Binzel 2019                    MITHNEOS Method: NIR


  28736 2000 GE133                    
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  28913 2000 OT                       
        Behrend 2003web                Period originally reported as 15.30 h.


  29075 1950 DA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  29292 Conniewalker                  
        Pravec 2011web                 Several possible tumbling solutions.


  29407 1996 UW                       
        Binzel 2019                    MITHNEOS Method: sVIS


  30105 2000 FO3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  30301 Kuditipudi                    
        Pravec 2019b                   Paired with (205231) 2000 QY110.


  30717 1937 UD                       
        Binzel 2019                    MITHNEOS Method: sVIS


  30786 Karkoschka                    
        Binzel 2019                    MITHNEOS Method: sVIS


  30825 1990 TG1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  31210 1998 BX7                      
        Binzel 2019                    MITHNEOS Method: VIS


  31221 1998 BP26                     
        Binzel 2019                    MITHNEOS Method: TAXON


  31345 1998 PG                       
        Binzel 2019                    MITHNEOS Method: VIS


  31346 1998 PB1                      
        Binzel 2019                    MITHNEOS Method: VIS


  31367 1998 WB9                      
        Binzel 2019                    MITHNEOS Method: sVIS


  31415 1999 AK23                     
        Binzel 2019                    MITHNEOS Method: VIS


  31669 1999 JT6                      
        Binzel 2019                    MITHNEOS Method: NIR


  31832 2000 AP59                     
        Binzel 2019                    MITHNEOS Method: sVIS


  31843 2000 CQ80                     
        Binzel 2019                    MITHNEOS Method: sVIS


  31869 2000 EF101                    
        Binzel 2019                    MITHNEOS Method: sVIS


  32122 2000 LD10                     
        Binzel 2019                    MITHNEOS Method: sVIS


  32575 2001 QY78                     
        Binzel 2019                    MITHNEOS Method: sVIS


  32827 1992 DF1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  32897 Curtharris                    
        Binzel 2019                    MITHNEOS Method: sVIS


  32906 1994 RH                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  32957 1996 HX20                     
        Pravec 2019b                   Paired with (38707) 2000 QK89.


  33046 1997 UF2                      
        Pravec 2014web                 P2 not determined. One attenuations seen, but unexplained.


  33325 1998 RH3                      
        Pravec 2019b                   Paired with 2012 AX10.


  33342 1998 WT24                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  33881 2000 JK66                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  34048 2000 OR35                     
        Binzel 2019                    MITHNEOS Method: sVIS


  34613 2000 UR13                     
        Binzel 2019                    MITHNEOS Method: TAXON


  34755 2001 QW120                    
        Binzel 2019                    MITHNEOS Method: sVIS


  35107 1991 VH                       
        Merline 2008                   AO observations separated primary and satellite. Angular
                                       separation of 0.08' (~3.1 km). Satellite ~2.0 mag fainter.
                                       Separation and size agree with Pravec (IAUC 6607).

        Binzel 2019                    MITHNEOS Method: VISNIR


  35368 1997 UB8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  35396 1997 XF11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  35432 1998 BG9                      
        Binzel 2019                    MITHNEOS Method: VIS


  35670 1998 SU27                     
        Binzel 2019                    MITHNEOS Method: VIS


  35783 1999 JU20                     
        Warner 2022g                   Some suspicious secondary periods between 2-5 h, but the
                                       lightcurve amplitude and noise are about the same.


  36017 1999 ND43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  36183 1999 TX16                     
        Binzel 2019                    MITHNEOS Method: VIS


  36284 2000 DM8                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  37336 2001 RM                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  37384 2001 WU1                      
        Binzel 2019                    MITHNEOS Method: NIR


  37424 2001 YA3                      
        Benishek 2021k                 An unexplained attenuation may be due to third body.


  38071 1999 GU3                      
        Binzel 2019                    MITHNEOS Method: NIR


  38079 1999 HF                       
        Pravec 2020web                 The amplitudes for the Pravec 2020web observation subsets are
                                       for outside the mutual events.


  38086 Beowulf                       
        Binzel 2019                    MITHNEOS Method: TAXON


  38184 1999 KF                       
        Pravec 2019b                   Paired with (221867) 2008 GR80.


  38707 2000 QK89                     
        Pravec 2019b                   Paired with (32957) 1996 HX20.


  39235 2000 YH55                     
        Binzel 2019                    MITHNEOS Method: sVIS


  39489 1981 EU6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  39565 1992 SL                       
        Binzel 2019                    MITHNEOS Method: NIR


  39572 1993 DQ1                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  39702 1996 TZ10                     
        Binzel 2019                    MITHNEOS Method: sVIS


  40267 1999 GJ4                      
        Binzel 2019                    MITHNEOS Method: VIS


  40310 1999 KU4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  40366 1999 NF27                     
        Pravec 2019b                   Paired with (78024) 2002 JO70.


  42355 Typhon                        
        Noll 2006a                     Ds/Dp: ~0.5, assuming same albedo for both bodies.

        Grundy 2008                    Orbit SMA: 1628 ± 29 km. Ds: 84 ± 16 km.

        Benecchi 2009                  See note under 2001 QC298.


  42887 1999 RV155                    
        Binzel 2019                    MITHNEOS Method: sVIS


  42946 1999 TU95                     
        Pravec 2019b                   Paired with (165548) 2001 DO37.


  43008 1999 UD31                     
        Pravec 2019b                   Paired with (441549) 2008 TM68.


  43017 1999 VA2                      
        Binzel 2019                    MITHNEOS Method: sVIS


  44200 1998 MJ25                     
        Binzel 2019                    MITHNEOS Method: sVIS


  44534 1998 YZ9                      
        Polishook 2012b                Authors gave P=22.5 h but with monomodal solution. The
                                       amplitude virtually assures a bimodal lightcurve with a
                                       period about double the stated value.


  44612 1999 RP27                     
        Pravec 2012web                 Period assumed from work in 2010.

        Pravec 2012web                 Period assumed from work in 2010.

        Pravec 2019b                   Paired with (2210) Moore-Sitterly.


  44619 1999 RO42                     
        Binzel 2019                    MITHNEOS Method: sVIS


  44620 1999 RS43                     
        Pravec 2019b                   Paired with (295745) 2008 UH98.


  45251 1999 YN                       
        Binzel 2019                    MITHNEOS Method: sVIS


  45991 2001 BQ70                     
        The Masi et al. paper gave this as a C-type on the basis of a neutral spectrum. However,
        given its location in the inner main belt, we adopted class X and a Pv = 0.18.


  46162 2001 FM78                     
        Pravec 2019b                   Paired with (323879) 2004 SA204.


  46829 McMahon                       
        Pravec 2019b                   Paired with 2014 VR4. Observing Circumstances are for
                                       lightcurves from 2015 Feb.


  47035 1998 WS                       
        Binzel 2019                    MITHNEOS Method: VIS


  47171 Lempo                         
        Benecchi 2009                  See note under 2001 QC298.


  47581 2000 AN178                    
        Binzel 2019                    MITHNEOS Method: NIR


  47648 2000 CA40                     
        Binzel 2019                    MITHNEOS Method: sVIS


  48468 1991 SS1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  48527 1993 LC1                      
        Pravec 2019b                   Paired with (25884) Asai.


  48603 1995 BC2                      
        Binzel 2019                    MITHNEOS Method: VIS


  48621 1995 OC                       
        Binzel 2019                    MITHNEOS Method: sVIS


  48652 1995 VB                       
        Pravec 2019b                   Paired with (139156) 2001 FP106.


  49791 1999 XF31                     
        Pravec 2019b                   Paired with (436459) 2011 CL97.


  50000 Quaoar                        
        Fraser 2013                    Period is for a non-zero eccentric orbit. A solution near
                                       298.3 h is possible assuming a zero eccentricity.


  50867 2000 GM4                      
        Binzel 2019                    MITHNEOS Method: sVIS


  51157 2000 HB57                     
        Binzel 2019                    MITHNEOS Method: sVIS


  51609 2001 HZ32                     
        Pravec 2019b                   Paired with (322672) 1999 TE221.


  51866 2001 PH3                      
        Pravec 2019b                   Paired with (326894) 2003 WV25.


  52340 1992 SY                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  52387 Huitzilopochtli               
        Binzel 2019                    MITHNEOS Method: NIR


  52750 1998 KK17                     
        Warner 2017c                   Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


  52760 1998 ML14                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


  52762 1998 MT24                     
        Binzel 2019                    MITHNEOS Method: eVISNIR


  52768 1998 OR2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  52773 1998 QU12                     
        Pravec 2019b                   Paired with (279865) 2001 HU24.


  52852 1998 RB75                     
        Pravec 2019b                   Paired with (250322) 2003 SC7.


  53319 1999 JM8                      
        Binzel 2019                    MITHNEOS Method: sVISNIR

        Skiff 2019b                    Mid-date is approximate. Additional data from October also
                                       available.


  53430 1999 TY16                     
        Binzel 2019                    MITHNEOS Method: NIR


  53431 1999 UQ10                     
        Warner 2010k                   A weak signal with a period of 38.4 h was found. If this is
                                       subtracted from the data, the scatter in the data was reduced
                                       significantly. There was insufficent evidence to attribute
                                       the signal to a specific cause.


  53435 1999 VM40                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  53537 Zhangyun                      
        Pravec 2019b                   Paired with (503955) 2004 ED107.


  53576 2000 CS47                     
        Pravec 2019b                   Paired with ((421781) 2014 QG22.


  53789 2000 ED104                    
        Binzel 2019                    MITHNEOS Method: NIR


  54041 2000 GQ113                    
        Pravec 2019b                   Paired with (220143) 2002 TO134.


  54071 2000 GQ146                    
        Binzel 2019                    MITHNEOS Method: NIR


  54509 YORP                          
        Lowry 2007a                    Date for phase is end of period: Jul 28, 2001 - Jul 27, 2002.
                                       Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Aug. 12, 2004 - Aug. 31,
                                       2005. Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Jul 27, 2002 - Aug. 27,
                                       2003. Paper proved spin up due to YORP effect.

        Lowry 2007a                    Date for phase is end of period: Jul. 29, 2003 - Sep. 11,
                                       2004. Paper proved spin up due to YORP effect.

        Taylor 2007                    Date for phase is for beginning of observations that spanned
                                       from 2001 - 2005. Diameter and spin axis were determined from
                                       radar observations. Paper proved spin up due to YORP effect.
                                       

        Binzel 2019                    MITHNEOS Method: NIR


  54660 2000 UJ1                      
        Binzel 2019                    MITHNEOS Method: TAXON


  54686 2001 DU8                      
        Binzel 2019                    MITHNEOS Method: VIS


  54690 2001 EB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  54789 2001 MZ7                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2023a                   Secondary period lightcurve resembles one for a slightly
                                       elongated body, i.e., there is a possiblity that this is a
                                       'very wide binary.'


  54827 Kurpfalz                      
        Pravec 2010a                   Paired with (6070) Rheinland.

        Pravec 2019b                   Paired with (6070) Rheinland.


  55532 2001 WG2                      
        Stephens 2014e                 Unique solution not possible. Second period for NPAR table is
                                       one of several contenders.

        Binzel 2019                    MITHNEOS Method: VIS


  55576 Amycus                        
        Thirouin 2010                  Number given as 55567, which is 2002 CS6. The LCDB authors
                                       presumed the name/designation were correct.


  55764 1992 DG12                     
        Pravec 2019b                   Unspecified other possible periods. Paried with (305693) 2009
                                       BB131.


  55913 1998 FL12                     
        Pravec 2019b                   Paired with 2005 GQ107.


  56048 1998 XV39                     
        Pravec 2019b                   Paired with (76148) 2000 EP17.


  56150 1999 CT103                    
        Originally Derm4l in Dermawan Ph.D. thesis.


  56232 1999 JM31                     
        Pravec 2019b                   Paired with (115978) 2003 WQ56.


  56700 2000 LL28                     
        Pravec 2019b                   Paired with (414166) 2008 AU67.


  57047 2001 LG1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  57202 2001 QJ53                     
        Pravec 2019b                   Paired with (276353) 2002 UY20.


  58046 2002 XA14                     
        Binzel 2019                    MITHNEOS Method: sVIS


  59184 1999 AR15                     
        Pravec 2019b                   Paired with (293667) 2007 PD19.


  59394 1999 FZ23                     
        Pravec 2019b                   Paired with (11286) 1990 RO8.


  60458 2000 CM114                    
        Grundy 2019b                   For Grundy 2019b, the spin axis values are for the orbital
                                       pole. The primary's pole will be the same or similar.


  60546 2000 EE85                     
        Pravec 2019b                   Paired with (88604) 2001 QH293.


  60677 2000 GO18                     
        Pravec 2019b                   Paired with (142131) 2002 RV11.


  60735 2000 GF82                     
        Binzel 2019                    MITHNEOS Method: sVIS


  60744 2000 GB93                     
        Pravec 2019b                   Paired with (218099) 2002 MH3.


  60924 2000 JF44                     
        Binzel 2019                    MITHNEOS Method: sVIS


  61461 2000 QA31                     
        Warner 2011o                   One-night stand. Solution is based on a half-period analysis.


  61799 2000 QC184                    
        Binzel 2019                    MITHNEOS Method: sVIS


  63047 2000 WQ93                     
        Pravec 2019b                   Paired with (393274) 2013 WJ82.


  63095 2000 WS142                    
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


  63160 2000 YN8                      
        Binzel 2019                    MITHNEOS Method: sVIS


  63164 2000 YU14                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  63291 2001 DU87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  63341 2001 FD77                     
        Binzel 2019                    MITHNEOS Method: sVIS


  63440 Rozek                         
        Pravec 2019b                   Paired with (331933) 2004 TV14.


  63583 2001 QP31                     
        Binzel 2019                    MITHNEOS Method: sVIS


  63970 2001 SG72                     
        Pravec 2019b                   Paired with 2013 CT63.


  65489 Ceto                          
        Benecchi 2009                  See note under 2001 QC298.


  65679 1989 UQ                       
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: VISNIR


  65706 1992 NA                       
        Binzel 2019                    MITHNEOS Method: VIS


  65733 1993 PC                       
        Binzel 2019                    MITHNEOS Method: NIR


  65784 Naderayama                    
        Binzel 2019                    MITHNEOS Method: NIR


  65803 Didymos                       
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Binzel 2019                    MITHNEOS Method: VISNIR


  65996 1998 MX5                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66008 1998 QH2                      
        Binzel 2019                    MITHNEOS Method: TAXON


  66063 1998 RO1                      
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Binzel 2019                    MITHNEOS Method: sVISNIR


  66146 1998 TU3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66251 1999 GJ2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  66272 1999 JW6                      
        Warner 2021d                   A third period of P3 = 15.99 h is likely due to diurnal
                                       systematics. It has no effect on the P1/P2 solutions save to
                                       remove some noise from each lightcurve.


  66358 1999 JW87                     
        Binzel 2019                    MITHNEOS Method: sVIS


  66391 Moshup                        
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Behrend 2018web                Apparent mutual event on 2018 June 7 (UT) but not mentioned.

        Behrend 2018web                No signs of known satellite.

        Behrend 2019web                Phased curve shows known satellite mutual events. No
                                       secondary period reported.

        Binzel 2019                    MITHNEOS Method: NIR


  66419 1999 NR13                     
        Binzel 2019                    MITHNEOS Method: sVIS


  66652 Borasisi                      
        Noll 2004                      Alternate solution: P = 1109.6 Ãƒâ€šÃ‚Â± 1.6 h.

        Benecchi 2009                  See note under 2001 QC298.

        Grundy 2011                    Orbital period determined from astrometric measurements.


  66659 1999 TJ1                      
        Pravec 2019b                   Paired with (446085) 2013 CW179.


  66959 1999 XO35                     
        Binzel 2019                    MITHNEOS Method: VIS


  67399 2000 PJ6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  67502 2000 RE44                     
        Binzel 2019                    MITHNEOS Method: sVIS


  67729 2000 UQ23                     
        Binzel 2019                    MITHNEOS Method: sVIS


  67865 2000 WG23                     
        Binzel 2019                    MITHNEOS Method: VIS


  68063 2000 YJ66                     
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2022b                   An additional period of 5.73 h suggests a third body in the
                                       system.


  68216 2001 CV26                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Stephens 2015g                 No satellite found with radar observations in 2009.

        Binzel 2019                    MITHNEOS Method: VISNIR


  68278 2001 FC7                      
        Binzel 2019                    MITHNEOS Method: sVIS

        Pravec 2019web                 Unexplained deviations on 2018 Jan 14, 20, and 24.


  68346 2001 KZ66                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   YORP detection: (8.43 Ã‚Â± 0.69)*10^-8 rad/day/day. Combinded
                                       optical and radar data. Original optical raw data available
                                       at https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/.

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   Original raw lightcurve data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/

        Zegmott 2021                   Original raw optical data available at
                                       https://cdsarc.cds.unistra.fr/ftp/J/MNRAS/507/4914/


  68350 2001 MK3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  68359 2001 OZ13                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  68372 2001 PM9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  68548 2001 XR31                     
        Binzel 2019                    MITHNEOS Method: VIS


  68950 2002 QF15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  69142 2003 FL115                    
        Pravec 2019b                   Paired with (127502) 2002 TP59.


  69230 Hermes                        
        Binzel 2019                    MITHNEOS Method: NIR


  69298 1992 DR9                      
        Paired with 2012 FF11.


  69311 Russ                          
        Binzel 2019                    MITHNEOS Method: sVIS


  69406 Martz-Kohl                    
        Warner 2011k                   If the shorter period is correct, this makes the asteroid a
                                       good binary candidate.


  70030 Margaretmiller                
        Warner 2012b                   No mutual events seen but independent observations from two
                                       locations show a secondary period of either 15.8 or 11.5 h.


  70511 1999 TL103                    
        Pravec 2019b                   Paired with (462176) 2007 TC334.


  71997 2000 WD178                    
        Binzel 2019                    MITHNEOS Method: sVIS


  72204 2000 YV133                    
        Binzel 2019                    MITHNEOS Method: sVIS


  72748 2001 FR126                    
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


  73735 1993 QE3                      
        Binzel 2019                    MITHNEOS Method: sVIS


  74096 1998 QD15                     
        Pravec 2019b                   Paired with (224857) 2006 YE45.


  74789 1999 SY5                      
        Binzel 2019                    MITHNEOS Method: sVIS


  76111 2000 DK106                    
        Pravec 2019b                   Paired with (354652) 2005 JY103.


  76148 2000 EP17                     
        Pravec 2019b                   Paired with (56048) 1998 XV39.


  76978 2001 BY60                     
        Binzel 2019                    MITHNEOS Method: sVIS


  77971 Donnolo                       
        Binzel 2019                    MITHNEOS Method: sVIS


  78024 2002 JO70                     
        Pravec 2019b                   Paired with (40366) 1999 NF 27.


  78085 2002 LV23                     
        Pravec 2023web                 Probably binary.  The solution for the two periods appears
                                       unique (but it is not clear which of them is the primary
                                       period).


  78587 2002 SZ12                     
        Binzel 2019                    MITHNEOS Method: sVIS


  79340 1996 TO41                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


  79360 Sila-Nunam                    
        Benecchi 2009                  See note under 2001 QC298.


  79576 1998 QG98                     
        Binzel 2019                    MITHNEOS Method: sVIS


  80218 1999 VO123                    
        Pravec 2019b                   Paired with (213471) 2002 ES90.


  80806 2000 CM105                    
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is for the
                                       combined light since the binary pair could not be resolved.


  82075 2000 YW134                    
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is for the
                                       combined light since the binary pair could not be resolved.


  82105 2001 FG26                     
        Binzel 2019                    MITHNEOS Method: sVIS


  82676 2001 PV23                     
        Binzel 2019                    MITHNEOS Method: sVIS


  84203 2002 RD133                    
        Pravec 2019b                   Paired with (285637) 2000 SS4.


  85182 1991 AQ                       
        Binzel 2019                    MITHNEOS Method: TAXON


  85185 Lederman                      
        Binzel 2019                    MITHNEOS Method: sVIS


  85236 1993 KH                       
        Binzel 2019                    MITHNEOS Method: NIR


  85274 1994 GH                       
        Binzel 2019                    MITHNEOS Method: sVIS


  85275 1994 LY                       
        Binzel 2019                    MITHNEOS Method: NIR

        Masiero 2020b                  The geocentric phase angle and PAB in the Masiero 2020b
                                       details records were computed using the mean MJD given in the
                                       file. H-G are the values used for the model and appear only
                                       in details records. The MPCORB H-G at the time of import are
                                       used in the summary line. The albedo error is the larger
                                       linear error listed in the table. The diameter is the
                                       corrected value (see Masiero et al. 2020b).


  85490 1997 SE5                      
        Binzel 2019                    MITHNEOS Method: TAXON


  85585 Mjolnir                       
        Binzel 2019                    MITHNEOS Method: NIR


  85709 1998 SG36                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  85713 1998 SS49                     
        Binzel 2019                    MITHNEOS Method: NIR


  85770 1998 UP1                      
        Binzel 2019                    MITHNEOS Method: NIR


  85774 1998 UT18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  85804 1998 WQ5                      
        Binzel 2019                    MITHNEOS Method: NIR


  85818 1998 XM4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  85839 1998 YO4                      
        Binzel 2019                    MITHNEOS Method: NIR


  85848 1998 YP29                     
        Binzel 2019                    MITHNEOS Method: sVIS


  85867 1999 BY9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  85938 1999 DJ4                      
        Binzel 2019                    MITHNEOS Method: VIS


  85953 1999 FK21                     
        Binzel 2019                    MITHNEOS Method: VIS


  85989 1999 JD6                      
        Aznar 2018b                    Published lightcurve is inverted, i.e., faintest when at top.

        Binzel 2019                    MITHNEOS Method: VISNIR


  85990 1999 JV6                      
        Giorgini 2016                  Yarkovsky detection.

        Binzel 2019                    MITHNEOS Method: VISNIR

        Giorgini 2019                  Yarkovsky detection. Replaces text in CBET 4279.

        Rozek 2019b                    Model is based on lightcurve/radar combination for a bilobed
                                       shape without a narrow 'neck.'


  86039 1999 NC43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  86067 1999 RM28                     
        Binzel 2019                    MITHNEOS Method: NIR


  86212 1999 TG21                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


  86324 1999 WA2                      
        Binzel 2019                    MITHNEOS Method: NIR


  86326 1999 WK13                     
        Binzel 2019                    MITHNEOS Method: VIS


  86450 2000 CK33                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  86626 2000 EV124                    
        Binzel 2019                    MITHNEOS Method: sVIS


  86667 2000 FO10                     
        Binzel 2019                    MITHNEOS Method: NIR


  86819 2000 GK137                    
        Binzel 2019                    MITHNEOS Method: VISNIR


  86829 2000 GR146                    
        Binzel 2019                    MITHNEOS Method: VIS


  87024 2000 JS66                     
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2021web                 A2 amplitude assumed to be same as A1.

        Warner 2022c                   Third period: 39.46 Â± 0.01, A = 0.13 Â± 0.02. See Pravec et
                                       al. (2021web).


  87311 2000 QJ1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  87510 2000 QJ183                    
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


  87684 2000 SY2                      
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021a                   P2 is not a rotational alias of P1 and so the ambiguity lies
                                       in explaining the two periods. The low amplitudes and nearly
                                       the same periods precludes these being periods of a tumbler.
                                       


  87887 2000 SS286                    
        Pravec 2019b                   Paried with (415992) 2002 AT49.


  88188 2000 XH44                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2021g                   Very wide binary candidate, but solution is very tenuous.


  88254 2001 FM129                    
        Binzel 2019                    MITHNEOS Method: VISNIR


  88259 2001 HJ7                      
        Pravec 2019b                   Paired with (337181) 1999 VA117.


  88604 2001 QH293                    
        Pravec 2019b                   Paired with (60546) 2000 EE85.


  88611 Teharonhiawako                
        Osip 2003                      Diameter is for primary if assuming density = 1.0 gcm^-3.
                                       Secondary diameter: 136 Ãƒâ€šÃ‚Â± 10 km.


  88666 2001 RP79                     
        Pravec 2019b                   Paired with (501710) 2014 UY23.


  88710 2001 SL9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


  88938 2001 TR33                     
        Binzel 2019                    MITHNEOS Method: sVIS


  89136 2001 US16                     
        Binzel 2019                    MITHNEOS Method: VIS


  89355 2001 VS78                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  89766 2002 AO62                     
        Binzel 2019                    MITHNEOS Method: sVIS


  89830 2002 CE                       
        Binzel 2019                    MITHNEOS Method: VIS


  89958 2002 LY45                     
        Binzel 2019                    MITHNEOS Method: NIR


  90075 2002 VU94                     
        Binzel 2019                    MITHNEOS Method: NIR


  90367 2003 LC5                      
        Binzel 2019                    MITHNEOS Method: NIR


  90403 2003 YE45                     
        Binzel 2019                    MITHNEOS Method: NIR


  90416 2003 YK118                    
        Binzel 2019                    MITHNEOS Method: NIR


  90482 Orcus                         
        Brown 2010                     The stated diameter is the effecitve size of the Orcus-Vanth
                                       system. Individual diameters are 900 and 280 km, assuming the
                                       desnities and albedos are the same. If Vanth's albedo is 0.5
                                       that of Orcus, the diameters are 860 and 380 km.  The
                                       semi-major axis of the satellite orbit is 8980 ± 20 km.

        Sickafoose 2019                Diameter assumes a spherical shape.


  92336 2000 GY81                     
        Pravec 2019b                   Paired with (143662) 2003 SP84.


  92359 2000 HC24                     
        Binzel 2019                    MITHNEOS Method: sVIS


  93040 2000 SG                       
        Binzel 2019                    MITHNEOS Method: sVIS


  93751 2000 WH1                      
        Binzel 2019                    MITHNEOS Method: sVIS


  94210 2001 BK33                     
        Binzel 2019                    MITHNEOS Method: sVIS


  95626 2002 GZ32                     
        Santos-Sanz 2020               Volume-equivalent diameter from 366x306x120 km.


  95711 2003 AK                       
        Pravec 2007web                 Period > 10h. 100 hr is one of several possible solutions.


  96011 2004 PD6                      
        Binzel 2019                    MITHNEOS Method: sVIS


  96189 Pygmalion                     
        Binzel 2019                    MITHNEOS Method: VISNIR


  96315 1997 AP10                     
        Binzel 2019                    MITHNEOS Method: NIR


  96562 1998 SZ138                    
        Binzel 2019                    MITHNEOS Method: sVIS


  96590 1998 XB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  97805 2000 OJ15                     
        Pravec 2019b                   Paired with (279230) 2009 UX122.


  98866 Giannabussolari               
        Pravec 2019b                   Paired with 2015 RV228.


  98891 2001 BK41                     
        Binzel 2019                    MITHNEOS Method: sVIS


  98943 2001 CC21                     
        Binzel 2019                    MITHNEOS Method: VISNIR

        Warner 2023e                   P1 = 5.0159 h is secure but requires subtracting two periods
                                       of unknown origin: P2 = 15.82(0.01), A2 = 1.30(0.03), P3 =
                                       11.26(0.02), A3 = 0.21(0.05)


  99248 2001 KY66                     
        Binzel 2019                    MITHNEOS Method: NIR


  99799 2002 LJ3                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


  99869 2002 PF46                     
        Binzel 2019                    MITHNEOS Method: sVIS


  99907 1989 VA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


  99913 1997 CZ5                      
        Binzel 2019                    MITHNEOS Method: VIS


  99935 2002 AV4                      
        Binzel 2019                    MITHNEOS Method: NIR


  99942 Apophis                       
        Licandro 2016b                 Diameter and albedo are the averages of the min/max values.

        Binzel 2019                    MITHNEOS Method: VISNIR


 100004 1983 VA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 100017 1989 TN2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 100085 1992 UY4                      
        Mueller 2011a                  H taken from another source.

        Binzel 2019                    MITHNEOS Method: NIR


 100316 1995 MM2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 100440 1996 PJ6                      
        Pravec 2019b                   Paired with 2011 SE164.


 100480 1996 UK                       
        Binzel 2019                    MITHNEOS Method: VIS


 100553 Dariofo                       
        Binzel 2019                    MITHNEOS Method: sVIS


 100756 1998 FM5                      
        Binzel 2019                    MITHNEOS Method: VIS

        Warner 2022i                   Final solution required P3=2.54 h, A=0.08 mag. Periods 2 and
                                       3 are artifacts of additive multi-period analysis.


 100926 1998 MQ                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 101027 1998 QL71                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101065 1998 RV11                     
        Pravec 2019b                   Paired with (368313) 2002 PY103.


 101402 1998 VG1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101429 1998 VF31                     
        Binzel 2019                    MITHNEOS Method: NIR


 101554 1999 AL4                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101703 1999 CA150                    
        Pravec 2019b                   Paired with (142694) 2002 TW243.


 101742 1999 FO7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101811 1999 JQ6                      
        Binzel 2019                    MITHNEOS Method: sVIS


 101818 1999 JD13                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101952 1999 RY31                     
        Binzel 2019                    MITHNEOS Method: sVIS


 101955 Bennu                         
        Binzel 2019                    MITHNEOS Method: VISNIR


 102528 1999 US3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 102803 1999 VA169                    
        Binzel 2019                    MITHNEOS Method: sVIS


 103055 1999 XR134                    
        Pravec 2019b                   Paired with 2008 UZ220.


 103067 1999 XA143                    
        Binzel 2019                    MITHNEOS Method: NIR


 103501 2000 AT245                    
        Binzel 2019                    MITHNEOS Method: sVIS


 103506 2000 BD1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 103732 2000 CO103                    
        Binzel 2019                    MITHNEOS Method: sVIS


 104444 2000 GR3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 105155 2000 NG26                     
        Warner 2012g                   Many possible periods.


 105158 2000 OL                       
        Binzel 2019                    MITHNEOS Method: sVIS


 105247 2000 QH3                      
        Pravec 2019b                   Paired with 2009 SZ67.


 105943 2000 SY233                    
        Binzel 2019                    MITHNEOS Method: sVIS


 106589 2000 WN107                    
        Binzel 2019                    MITHNEOS Method: sVIS


 108182 2001 HY13                     
        Binzel 2019                    MITHNEOS Method: sVIS


 108410 2001 KG32                     
        Binzel 2019                    MITHNEOS Method: sVIS


 108519 2001 LF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 108522 2001 LQ                       
        Binzel 2019                    MITHNEOS Method: sVIS


 108663 2001 NE21                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 109077 2001 QR25                     
        Binzel 2019                    MITHNEOS Method: sVIS


 109226 2001 QH91                     
        Binzel 2019                    MITHNEOS Method: sVIS


 112221 2002 KH4                      
        Warner 2019p                   The binaries table gives P1 = 2.479 h and Ds/Dp >= 0.22. The
                                       P1 solution is extremely weak.


 112249 2002 LM9                      
        Pravec 2019b                   Paired with (261878) 2006 GR49.


 112985 2002 RS28                     
        Binzel 2019                    MITHNEOS Method: NIR


 114553 2003 BH42                     
        Binzel 2019                    MITHNEOS Method: sVIS


 114924 2003 QL41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 115978 2003 WQ56                     
        Pravec 2019b                   Paired with (56232) 1999 JM31.


 117306 2004 VF21                     
        Pravec 2019b                   Paired with (10123) Fideoja.


 118112 2665 T-3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 119067 2001 KP76                     
        Marchis 2008a                  No lightcurves per se. Hubble observations show a binary
                                       system with components about the same size separated by
                                       0'.29, or about 8200 km.


 119979 2002 WC19                     
        Benecchi 2009                  See note under 2001 QC298. In this case, V-I is the combined
                                       light since the binary pair could not be resolved.


 120347 Salacia                       
        Noll 2006e                     Satellite 2.3 mag fainter.

        Stansberry 2012                SMAxis of orbit: 5619 ± 87 km. Individual diameters: Primary:
                                       905 ± 103 km; Secondary: 303 ± 35 km.


 120352 Gordonwong                    
        Binzel 2019                    MITHNEOS Method: sVIS


 120450 1982 SV                       
        Binzel 2019                    MITHNEOS Method: sVIS


 120578 1995 QV12                     
        Warner 2014f                   Large zero-point offsets required to get period. Could be
                                       signs of tumbling.


 121210 1999 QG2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 122011 2000 GL28                     
        Originally Derm8f in Dermawan Ph.D. thesis.


 122173 2000 KC28                     
        Pravec 2019b                   Paired with (259585) 2003 UG220.


 122421 2000 QZ101                    
        Binzel 2019                    MITHNEOS Method: sVIS


 124146 2001 MQ12                     
        Binzel 2019                    MITHNEOS Method: sVIS


 124200 2001 OM81                     
        Binzel 2019                    MITHNEOS Method: sVIS


 125475 2001 WA15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 129493 1995 BM2                      
        Binzel 2019                    MITHNEOS Method: VIS


 129541 1996 PQ9                      
        Binzel 2019                    MITHNEOS Method: sVIS


 129737 1999 AA9                      
        Binzel 2019                    MITHNEOS Method: sVIS


 130778 2000 SX369                    
        Pravec 2015web                 Possible second period.


 131045 2000 YH32                     
        Binzel 2019                    MITHNEOS Method: VIS


 133027 2002 XJ4                      
        Binzel 2019                    MITHNEOS Method: sVIS


 133090 2003 MS9                      
        Michimani 2023                 Result using two data sets: 2021 Oct an 2021 Dec.


 133531 2003 TJ5                      
        Binzel 2019                    MITHNEOS Method: sVIS


 134340 Pluto                         
        Tholen 1997                    The diameter of 2700 km is the effective diameter of the
                                       Pluto/Charon system based on Pv and H.  Pluto: D = 2350 ± 50
                                       km.  Charon (primary satellite): D = 1250 ± 50 km  Nix
                                       (S/2005 P1): Sep: 48700 km. D ~ 46 km  Hydra (S/2005 P2): Sep
                                       64800 km. D ~ 61 km.


 134371 1995 RH                       
        Binzel 2019                    MITHNEOS Method: sVIS


 134422 1998 QM3                      
        Warner 2015d                   The periods are two of several sets of solutions.


 134509 1999 FC8                      
        Binzel 2019                    MITHNEOS Method: sVIS


 134860 2000 OJ67                     
        Benecchi 2009                  See note under 2001 QC298.


 136108 Haumea                        
        Lellouch 2010                  Visible and Thermal observations.

        Lockwood 2014                  Ellipsoid lengths: a = 960 km, b = 770 km, c = 495 km.

        Dunham 2019                    Diameter computed from volume of ellipsoid with (abc) =
                                       (1050,840,537) km.


 136472 Makemake                      
        Lim 2010                       A dark area has 0.02 < p_v < 0.12 and 310 < D_eff < 380 km.


 136564 1977 VA                       
        Binzel 2019                    MITHNEOS Method: NIR


 136582 1992 BA                       
        This note applies to all entries for Masiero et al. (2020a). The albedo error is the listed
        maximum possible value when converting albedo values from log space to value space. The
        phase angle in the details record is from the file since the actual date of observation was
        not given. The value for H is the 'model-out' value, which may differ slightly from the
        value used in the NEATM modeling (the value given in Tables 1-4). This maintains full
        agreement with the listed albedo and diameter. See Masiero et al. (2020a) for details about
        assumed errors in H and G.


 136617 1994 CC                       
        Brozovic 2009b                 Estimated sizes: S1 > 100 m; S2 > 5 m.

        Brozovic 2011                  Inner satellite: D = 113 ± 30 m. P = 26 ± 12 h. P_orb =
                                       29.832 ± 2.400 h.   Outer satellite: D = 80 ± 30m. P = 14 ±
                                       7h. P_orb = 201.024 ± 12.0 h.

        Binzel 2019                    MITHNEOS Method: VISNIR


 136618 1994 CN2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 136745 1995 WL8                      
        Binzel 2019                    MITHNEOS Method: VIS


 136770 1996 PC1                      
        Binzel 2019                    MITHNEOS Method: NIR


 136793 1997 AQ18                     
        Binzel 2019                    MITHNEOS Method: VIS


 136795 Tatsunokingo                  
        Binzel 2019                    MITHNEOS Method: VIS


 136818 Selqet                        
        Binzel 2019                    MITHNEOS Method: TAXON


 136839 1997 WT22                     
        The geocentric phase angle and PAB in the Masiero 2020b details records were computed using
        the mean MJD given in the file. H-G are the values used for the model and appear only in
        details records. The MPCORB H-G at the time of import are used in the summary line. The
        albedo error is the larger linear error listed in the table. The diameter is the corrected
        value (see Masiero et al. 2020b).


 136849 1998 CS1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 136923 1998 JH2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 136993 1998 ST49                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 137032 1998 UO1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 137052 Tjelvar                       
        Binzel 2019                    MITHNEOS Method: VIS


 137062 1998 WM                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 137064 1998 WP5                      
        Binzel 2019                    MITHNEOS Method: VIS


 137069 1998 WQ15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 137084 1998 XS16                     
        Binzel 2019                    MITHNEOS Method: NIR


 137125 1999 CT3                      
        Binzel 2019                    MITHNEOS Method: NIR


 137126 1999 CF9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 137158 1999 FB                       
        Binzel 2019                    MITHNEOS Method: VIS


 137170 1999 HF1                      
        Warner 2016n                   No indications of known satellite.

        Binzel 2019                    MITHNEOS Method: VISNIR


 137199 1999 KX4                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 137230 1999 RG22                     
        Binzel 2019                    MITHNEOS Method: sVIS


 137427 1999 TF211                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 137671 1999 XP35                     
        Binzel 2019                    MITHNEOS Method: NIR


 137799 1999 YB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 137805 1999 YK5                      
        Binzel 2019                    MITHNEOS Method: sVIS


 137924 2000 BD19                     
        Binzel 2019                    MITHNEOS Method: NIR


 137925 2000 BJ19                     
        Binzel 2019                    MITHNEOS Method: VIS


 138013 2000 CN101                    
        Binzel 2019                    MITHNEOS Method: sVIS


 138127 2000 EE14                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138131 2000 ES20                     
        Binzel 2019                    MITHNEOS Method: sVIS


 138155 2000 ES70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138175 2000 EE104                    
        Binzel 2019                    MITHNEOS Method: NIR


 138205 2000 EZ148                    
        Binzel 2019                    MITHNEOS Method: TAXON


 138258 2000 GD2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138325 2000 GO82                     
        Binzel 2019                    MITHNEOS Method: VIS


 138404 2000 HA24                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138524 2000 OJ8                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138846 2000 VJ61                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138852 2000 WN10                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 138883 2000 YL29                     
        Binzel 2019                    MITHNEOS Method: NIR

        Skiff 2019b                    Lightcurve shape is similar to one produced by a satellite
                                       with mutual events. If so, Ds/Dp ~ 0.38.


 138893 2000 YH66                     
        Binzel 2019                    MITHNEOS Method: VIS


 138911 2001 AE2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 138937 2001 BK16                     
        Binzel 2019                    MITHNEOS Method: TAXON


 138947 2001 BA40                     
        Binzel 2019                    MITHNEOS Method: NIR


 138971 2001 CB21                     
        Period from Warner/Stephens is based on the combined data set. See independent entries in
        details tables for the two dates.

        Binzel 2019                    MITHNEOS Method: VIS

        Pravec 2022web                 Longer period is not formally excluded but is less likely.

        Warner 2022f                   Based on data from 2022 Feb 27 and 28


 139056 2001 FY                       
        Binzel 2019                    MITHNEOS Method: VIS


 139156 2001 FP106                    
        Pravec 2019b                   Paired with (48652) 1995 VB.


 139345 2001 KA67                     
        Stephens 2018j                 Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


 139359 2001 ME1                      
        Binzel 2019                    MITHNEOS Method: NIR


 139537 2001 QE25                     
        Pravec 2019b                   Paired with (210904) 2001 SR218.


 139622 2001 QQ142                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 139775 2001 QG298                    
        Lacerda 2011                   The paper presumes a 'contact binary.' However, the
                                       lightcurves presented do not show the obvious indicators of
                                       'shoulders' in the descending and ascending branches. The
                                       lightcurve can be equally explained by a simple,
                                       highly-elongated body.


 140039 2001 SO73                     
        Binzel 2019                    MITHNEOS Method: NIR


 141018 2001 WC47                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 141052 2001 XR1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 141079 2001 XS30                     
        Binzel 2019                    MITHNEOS Method: VIS


 141354 2002 AJ29                     
        Binzel 2019                    MITHNEOS Method: sVIS


 141424 2002 CD                       
        Binzel 2019                    MITHNEOS Method: NIR


 141432 2002 CQ11                     
        Binzel 2019                    MITHNEOS Method: NIR


 141484 2002 DB4                      
        Binzel 2019                    MITHNEOS Method: VIS


 141498 2002 EZ16                     
        Binzel 2019                    MITHNEOS Method: NIR


 141593 2002 HK12                     
        Binzel 2019                    MITHNEOS Method: NIR


 141670 2002 JS100                    
        Warner 2018a                   Period of 4.719 h cannot be formally excluded, but is not
                                       likely.


 142040 2002 QE15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 142131 2002 RV11                     
        Pravec 2019b                   Paired with (60677) 2000 GO18.


 142348 2002 RX211                    
        Binzel 2019                    MITHNEOS Method: NIR


 142464 2002 TC9                      
        Binzel 2019                    MITHNEOS Method: NIR


 142555 2002 TB58                     
        Binzel 2019                    MITHNEOS Method: VIS


 142561 2002 TX68                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 142694 2002 TW243                    
        Pravec 2019b                   Paired with (101703) 1999 CA150.


 142781 2002 UM11                     
        Warner 2014e                   Multiple solutions possible due to the nearly flat
                                       lightcurve.


 143381 2003 BC21                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 143487 2003 CR20                     
        Binzel 2019                    MITHNEOS Method: NIR


 143624 2003 HM16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 143651 2003 QO104                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 143662 2003 SP84                     
        Pravec 2019b                   Paired with (92336) 2000 GY81.


 143947 2003 YQ117                    
        Binzel 2019                    MITHNEOS Method: NIR


 144411 2004 EW9                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 144898 2004 VD17                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 144900 2004 VG64                     
        Binzel 2019                    MITHNEOS Method: NIR


 144901 2004 WG1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 144922 2005 CK38                     
        Binzel 2019                    MITHNEOS Method: NIR


 145656 4788 P-L                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 145720 1993 OX7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 147431 2003 JA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 148480 2001 FE155                    
        Binzel 2019                    MITHNEOS Method: sVIS


 148780 Altjira                       
        Grundy 2011                    Orbital period determined from astrometric measurements.


 149592 2004 CU51                     
        Binzel 2019                    MITHNEOS Method: sVIS


 150398 2000 EC59                     
        Originally Derm1e in Dermawan Ph.D. thesis.


 152558 1990 SA                       
        Binzel 2019                    MITHNEOS Method: NIR


 152560 1991 BN                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 152563 1992 BF                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 152627 1997 DF                       
        Binzel 2019                    MITHNEOS Method: NIR


 152637 1997 NC1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 152664 1998 FW4                      
        Binzel 2019                    MITHNEOS Method: NIR


 152679 1998 KU2                      
        Binzel 2019                    MITHNEOS Method: VIS


 152742 1998 XE12                     
        Binzel 2019                    MITHNEOS Method: TAXON


 152754 1999 GS6                      
        Binzel 2019                    MITHNEOS Method: NIR


 152756 1999 JV3                      
        Binzel 2019                    MITHNEOS Method: NIR


 152770 1999 RR28                     
        Binzel 2019                    MITHNEOS Method: NIR


 152858 1999 XN35                     
        Hills 2013b                    Several possible solutions for P_Orb, ranging from 11 to 36
                                       h, if the deviations are due to a satellite.


 152895 2000 CQ101                    
        Binzel 2019                    MITHNEOS Method: NIR


 152931 2000 EA107                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 152964 2000 GP82                     
        Binzel 2019                    MITHNEOS Method: sVIS


 152978 2000 GJ147                    
        Binzel 2019                    MITHNEOS Method: VIS


 153002 2000 JG5                      
        Binzel 2019                    MITHNEOS Method: VIS


 153201 2000 WO107                    
        Binzel 2019                    MITHNEOS Method: VIS


 153219 2000 YM29                     
        Binzel 2019                    MITHNEOS Method: NIR


 153591 2001 SN263                    
        Becker 2008                    Density (Primary): 1.2 ± 0.4 g/cm^3

        Nolan 2008                     Radar observations show three objects in the 2001 SN263
                                       system. Estimated sizes are 2 km, 1 km, and 0.400 km.

        Becker 2015b                   Dp: 2.5 ± 0.3 km; Ds1: 0.77 ± 0.12 km; Ds2: 0.43 ± 0.14 km.
                                       Porb1: 16.464 ± 0.048; Porb2: 150 ± 3 h.

        Binzel 2019                    MITHNEOS Method: sVISNIR


 153814 2001 WN5                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 153842 2001 XT30                     
        Binzel 2019                    MITHNEOS Method: NIR


 153953 2002 AD9                      
        Binzel 2019                    MITHNEOS Method: VIS


 153958 2002 AM31                     
        Binzel 2019                    MITHNEOS Method: TAXON


 154029 2002 CY46                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 154244 2002 KL6                      
        Binzel 2019                    MITHNEOS Method: NIR


 154276 2002 SY50                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 154278 2002 TB9                      
        Binzel 2019                    MITHNEOS Method: VIS


 154302 2002 UQ3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 154347 2002 XK4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 154453 2003 CJ11                     
        Binzel 2019                    MITHNEOS Method: NIR


 154555 2003 HA                       
        Binzel 2019                    MITHNEOS Method: sVIS


 154634 2003 XX38                     
        Pravec 2019b                   Paired with (7343) Ockeghem.


 154715 2004 LB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 154828 2004 RT8                      
        Pravec 2019b                   Paired with (13284) 1998 QB52.


 155140 2005 UD                       
        Binzel 2019                    MITHNEOS Method: sVIS

        Huang 2021                     G is for G1. G2 = -0.006 Ãƒâ€šÃ‚Â± 0.006


 155334 2006 DZ169                    
        Binzel 2019                    MITHNEOS Method: sVISNIR


 156032 2001 RP142                    
        Binzel 2019                    MITHNEOS Method: sVIS


 156294 2001 WU66                     
        Chang 2021                     This note applies to all Chang 2021 (PSJ 2) entries. The
                                       observations were made in g and r2 bands. The photometric
                                       bands (for H) were assigned as SG and SR, respectively. The
                                       H_SR values were transformed to approximate V by using the
                                       LCDB V = SR+ 0.22. While not exact, this makes the values
                                       more compatible to H_V when plotting frequency-diameters. For
                                       diameter calculations, an albedo of 0.05 and G = 0.15 Ã‚Â±
                                       0.2 was assumed for both bands. Only some of the 53 objects
                                       could be tied to an object in the MPC database. For those
                                       without ID, and where possible, the phase and phase angle
                                       bisector values were assumed to be the same as for an
                                       identified object in the same observing block. The entries
                                       are flagged as being from a Sparse Wide-field Survey (SWF).


 157995 2000 LF26                     
        Binzel 2019                    MITHNEOS Method: sVIS


 158853 2004 NJ32                     
        Binzel 2019                    MITHNEOS Method: sVIS


 159111 2004 VG15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 159368 1979 QB                       
        Binzel 2019                    MITHNEOS Method: sVIS


 159402 1999 AP10                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 159493 2000 UA                       
        Binzel 2019                    MITHNEOS Method: NIR


 159533 2001 HH31                     
        Binzel 2019                    MITHNEOS Method: NIR


 159609 2002 AQ3                      
        Binzel 2019                    MITHNEOS Method: VIS


 159635 2002 CZ46                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 159857 2004 LJ1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 159882 2004 RQ289                    
        Binzel 2019                    MITHNEOS Method: sVIS


 159898 2004 TO216                    
        Binzel 2019                    MITHNEOS Method: sVIS


 160091 2000 OL67                     
        Marchis 2008a                  No lightcurve per se. Hubble observations show a binary
                                       system with the components separated by 0'.29, or about 7800
                                       km. The secondary was about 0.6m fainter than the primary.


 160092 2000 PL6                      
        Binzel 2019                    MITHNEOS Method: sVIS


 160137 2001 BU41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 160519 1995 CS3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 161989 Cacus                         
        Durech 2018a                   YORP detection.

        Binzel 2019                    MITHNEOS Method: NIR


 161998 1988 PA                       
        Franco 2011web                 Author gave P = 6.70 h for a monomodal solution. The
                                       amplitude virtually assures a bimodal curve and, therefore,
                                       double the reported period.

        Binzel 2019                    MITHNEOS Method: sVISNIR


 162000 1990 OS                       
        Binzel 2019                    MITHNEOS Method: VIS


 162011 Konnohmaru                    
        Binzel 2019                    MITHNEOS Method: VIS


 162015 1994 TF2                      
        Binzel 2019                    MITHNEOS Method: VIS


 162038 1996 DH                       
        Binzel 2019                    MITHNEOS Method: sVIS


 162058 1997 AE12                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162117 1998 SD15                     
        Binzel 2019                    MITHNEOS Method: NIR


 162142 1998 VR                       
        Binzel 2019                    MITHNEOS Method: VIS


 162149 1998 YQ11                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162157 1999 CV8                      
        Binzel 2019                    MITHNEOS Method: VIS


 162173 Ryugu                         
        Binzel 2019                    MITHNEOS Method: VISNIR

        Watanabe 2019                  Diameter is equatorial. Polar is 872 m. Spherical equivalent
                                       is D = 0.955 km.


 162181 1999 LF6                      
        Binzel 2019                    MITHNEOS Method: NIR


 162186 1999 OP3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 162361 2000 AF6                      
        Warner 2019m                   The solution for the secondary period (14.654 h) is very weak
                                       but its subtraction significantly lowers the RMS of the fit
                                       for the primary period.


 162385 2000 BM19                     
        Binzel 2019                    MITHNEOS Method: VIS


 162421 2000 ET70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 162422 2000 EV70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 162483 2000 PJ5                      
        Polishook 2008a                P_orb = 56.6 h is also possible.

        Binzel 2019                    MITHNEOS Method: VISNIR


 162510 2000 QW69                     
        The albedo error given for Masiero 2017 is the maximum possible value when converting from
        albedo values from log space to value space.


 162566 2000 RJ34                     
        Binzel 2019                    MITHNEOS Method: NIR


 162567 2000 RW37                     
        Binzel 2019                    MITHNEOS Method: VIS


 162581 2000 SA10                     
        Binzel 2019                    MITHNEOS Method: NIR


 162635 2000 SS164                    
        Binzel 2019                    MITHNEOS Method: NIR


 162740 2000 WF6                      
        Binzel 2019                    MITHNEOS Method: VIS


 162781 2000 XL44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 162785 2000 YA17                     
        Binzel 2019                    MITHNEOS Method: sVIS


 162900 2001 HG31                     
        Pravec 2008web                 Pravec analysis based on data from Warner 2009f and from
                                       Lowell Observatory (unpublished).

        Binzel 2019                    MITHNEOS Method: NIR


 162903 2001 JV2                      
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 162911 2001 LL5                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 162998 2001 SK162                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 163000 2001 SW169                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 163001 2001 SE170                    
        Binzel 2019                    MITHNEOS Method: NIR


 163014 2001 UA5                      
        Binzel 2019                    MITHNEOS Method: VIS


 163081 2002 AG29                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163132 2002 CU11                     
        Binzel 2019                    MITHNEOS Method: NIR


 163191 2002 EQ9                      
        Binzel 2019                    MITHNEOS Method: NIR


 163243 2002 FB3                      
        Binzel 2019                    MITHNEOS Method: NIR


 163249 2002 GT                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 163250 2002 GH1                      
        Binzel 2019                    MITHNEOS Method: NIR


 163364 2002 OD20                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163468 2002 RZ177                    
        Warner 2023f                   Peirod derived from a best-fit of the half-period.


 163692 2003 CY18                     
        Binzel 2019                    MITHNEOS Method: sVIS

        Warner 2022i                   Periods 2 and 3 are artifacts of additive multi-period
                                       analysis.


 163693 Atira                         
        Rivera-Valentin 2017           Diameter is that estimated for the primary. The satellite
                                       diameter is 1.0 ±0.3 km

        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       45.2-97.3 deg. The H_SR values are the linear extrapolation
                                       using the phase slope (beta_SR) of 0.03584. The lack of low
                                       phase angles prevented use of H-G or HG1,G2 modeling.


 163697 2003 EF54                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 163732 2003 KP2                      
        Binzel 2019                    MITHNEOS Method: VIS


 163899 2003 SD220                    
        Binzel 2019                    MITHNEOS Method: NIR

        Bondarenko 2019b               Diameter is for an effective spherical shape based on
                                       2700x1100 m a/b axis estimates.


 164121 2003 YT1                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: NIR


 164184 2004 BF68                     
        Binzel 2019                    MITHNEOS Method: TAXON


 164202 2004 EW                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 164206 2004 FN18                     
        Binzel 2019                    MITHNEOS Method: NIR


 164211 2004 JA27                     
        Binzel 2019                    MITHNEOS Method: NIR


 164214 2004 LZ11                     
        Binzel 2019                    MITHNEOS Method: sVIS


 164222 2004 RN9                      
        Binzel 2019                    MITHNEOS Method: NIR


 164400 2005 GN59                     
        Binzel 2019                    MITHNEOS Method: NIR


 164670 1996 XM6                      
        Binzel 2019                    MITHNEOS Method: NIR


 165389 2000 WC188                    
        Pravec 2019b                   Paired with 2011 SE164.


 165394 2000 XC15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 165548 2001 DO37                     
        Pravec 2019b                   Paired with (42946) 1999 TU95. Observing Circumstances for
                                       when Sloan color measurements from Lowell Observatory were
                                       made.


 167405 2003 WP118                    
        Pravec 2019b                   Paired with 2012 TK84.


 168315 1982 RA1                      
        Binzel 2019                    MITHNEOS Method: sVIS


 168378 1997 ET30                     
        Binzel 2019                    MITHNEOS Method: NIR


 168710 2000 HE41                     
        Binzel 2019                    MITHNEOS Method: sVIS


 168889 2000 WM95                     
        Binzel 2019                    MITHNEOS Method: VIS


 169660 2002 JG66                     
        Binzel 2019                    MITHNEOS Method: sVIS


 169675 2002 JM97                     
        Binzel 2019                    MITHNEOS Method: NIR


 170086 2002 XR14                     
        Binzel 2019                    MITHNEOS Method: NIR


 170172 2003 HV7                      
        Binzel 2019                    MITHNEOS Method: sVIS


 170502 2003 WM7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 170880 2004 PH85                     
        Binzel 2019                    MITHNEOS Method: sVIS


 170891 2004 TY16                     
        Binzel 2019                    MITHNEOS Method: NIR


 171677 2000 QG136                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 224 = 2000 QG136. TALCS 1238 = 171677.


 171730 2000 WX50                     
        Binzel 2019                    MITHNEOS Method: NIR


 171784 2001 BV67                     
        Binzel 2019                    MITHNEOS Method: sVIS


 171839 2001 JM1                      
        Binzel 2019                    MITHNEOS Method: VIS


 172678 2003 YM137                    
        Binzel 2019                    MITHNEOS Method: VIS


 173154 1996 ME                       
        Binzel 2019                    MITHNEOS Method: sVIS


 173689 2001 PK9                      
        Binzel 2019                    MITHNEOS Method: NIR


 173885 2001 UA61                     
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 158 = 2001 UA61. TALCS 1699 = 173885.


 173974 2001 XV127                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 200 = 2001 VV127. TALCS 1054 = 173974.


 173991 2001 XR170                    
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 249 = 2001 XR170. TALCS 2205 = 173991.


 174567 Varda                         
        Grundy 2015                    Periods are based on Orbit1 solution. Diameters: Varda 722 ±
                                       82; Ilmare 326 ± 38.


 175047 2004 FK93                     
        Masiero 2009                   The asteroid appears to have been independently analyzed
                                       twice in the TALCS survey, each time under a different MPC
                                       designation. TALCS 152 = 2004 FK93. TALCS 1699 = 175047.


 175706 1996 FG3                      
        Scheirich 2009                 Satellite:primary size ratio (D2/D1): 0.28 ± 0.02.
                                       Orbit:primary diameter ratio (a/A1): 3.1 ± 0.9.

        Mueller 2011a                  H and G taken from other sources.

        Wolters 2011                   D_sat = 0.51 0.03, assuming the same albedo as the primary.

        Scheirich 2015                 Data covered multipl apparitions from 1999-2013.

        Binzel 2019                    MITHNEOS Method: VISNIR


 175729 1998 BB10                     
        Binzel 2019                    MITHNEOS Method: VIS


 177255 2003 WC25                     
        Binzel 2019                    MITHNEOS Method: sVIS


 179806 2002 TD66                     
        Binzel 2019                    MITHNEOS Method: TAXON


 180186 2003 QZ30                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 181563 2006 UQ329                    
        For Yeh 2020, the amplitude error was found with max(0.01, 0.1*YehAmp)


 181882 1999 RF14                     
        The given period is for an obvious short-term period in the raw data, which - on the whole -
        show a steady brightening over the observations. This could either be a tumbler or a very
        wide binary.

        Skiff 2023                     The given period is for an obvious short-term period in the
                                       raw data, which - on the whole - show a steady brightening
                                       over the observations. This could either be a tumbler or a
                                       very wide binary.


 182259 2001 FZ185                    
        Pravec 2019b                   Paired with (289y) Ole Romer.


 184266 2004 VW14                     
        Binzel 2019                    MITHNEOS Method: NIR


 184990 2006 KE89                     
        Warner 2020j                   The 2+ rating is a combination of a U=2 for the primary and
                                       U=3 for the secondary period.


 185851 2000 DP107                    
        The Schierich (2009) results use previous lightcurve data to model the satellite:primary
        size ratio (D2/D1), pole of the orbital plane, and sidereal period of the orbit. The spin
        axis pole of the primary is considered to be the same as that of the orbit, i.e., the orbit
        lies in the primary's equatorial plane.

        Margot 2000                    Estimated diameters: 800 m and 300 m.

        Ostro 2000b                    Radar images show separations up to at least 1 km between
                                       components.

        Pravec 2000e                   Lightcurve observations confirmed binary nature discovered by
                                       radar.

        Scheirich 2009                 Solution 1: Satellite:primary size ratio (D2/D1): 0.43 ± 0.3.
                                       Orbit:primary diameter ratio (a/A1): 5.0 ± 2.0. Orbit period
                                       (sidereal): 42.09 ± 0.13  Solution 2: Satellite:primary size
                                       ratio (D2/D1): 0.43 ± 0.2. Orbit:primary diameter ratio
                                       (a/A1): 4.9 ± 1.2. Orbit period (sidereal): 42.79 ± 0.11

        Binzel 2019                    MITHNEOS Method: NIR


 187026 2005 EK70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 187737 2153 P-L                      
        Binzel 2019                    MITHNEOS Method: sVIS


 188452 2004 HE62                     
        Binzel 2019                    MITHNEOS Method: NIR


 189040 2000 MU1                      
        Binzel 2019                    MITHNEOS Method: VIS


 189494 1999 YY3                      
        Binzel 2019                    MITHNEOS Method: VIS


 189552 2000 RL77                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 190208 2006 AQ                       
        Warner 2015g                   No events seen and not likely so because of the long second
                                       period. The long period is attributed to the primary body
                                       while the short period is presumed to be due to the rotation
                                       of the fully asynchronous satellite.

        Binzel 2019                    MITHNEOS Method: NIR


 190491 2000 FJ10                     
        Binzel 2019                    MITHNEOS Method: VIS


 192559 1998 VO                       
        Binzel 2019                    MITHNEOS Method: TAXON


 192563 1998 WZ6                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 194006 2001 SG10                     
        Binzel 2019                    MITHNEOS Method: VIS


 194268 2001 UY4                      
        Binzel 2019                    MITHNEOS Method: VIS


 194386 2001 VG5                      
        Binzel 2019                    MITHNEOS Method: VIS


 196299 2003 FN1                      
        Binzel 2019                    MITHNEOS Method: NIR


 197994 2004 RG165                    
        Binzel 2019                    MITHNEOS Method: NIR


 198856 2005 LR3                      
        Binzel 2019                    MITHNEOS Method: NIR


 199003 2005 WJ56                     
        Binzel 2019                    MITHNEOS Method: NIR


 200754 2001 WA25                     
        Binzel 2019                    MITHNEOS Method: VIS


 200840 2001 XN254                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 202079 2004 SR39                     
        Binzel 2019                    MITHNEOS Method: sVIS


 203015 1999 YF3                      
        Binzel 2019                    MITHNEOS Method: VIS


 203471 2002 AU4                      
        Binzel 2019                    MITHNEOS Method: NIR


 203489 2002 AL80                     
        Pravec 2019b                   Paired with (17288) 2000 NZ10.


 205231 2000 QY110                    
        Pravec 2019b                   Paired with (30301) Kuditipudi.


 205383 2001 BV47                     
        Pravec 2019b                   Paired with (23998) 1999 RP29.


 205640 2001 XQ4                      
        Binzel 2019                    MITHNEOS Method: NIR


 205698 Troiani                       
        Binzel 2019                    MITHNEOS Method: NIR


 205744 2002 BK25                     
        Binzel 2019                    MITHNEOS Method: VIS


 206910 2004 NL8                      
        Binzel 2019                    MITHNEOS Method: NIR


 207398 2006 AS2                      
        Binzel 2019                    MITHNEOS Method: TAXON


 207408 2006 BY172                    
        Binzel 2019                    MITHNEOS Method: NIR


 207945 1991 JW                       
        Binzel 2019                    MITHNEOS Method: NIR


 207970 1996 BZ3                      
        Binzel 2019                    MITHNEOS Method: VIS


 208023 1999 AQ10                     
        Binzel 2019                    MITHNEOS Method: TAXON


 210482 1996 RW1                      
        Binzel 2019                    MITHNEOS Method: VIS


 210904 2001 SR218                    
        Pravec 2019b                   Paired with (139537) 2001 QE25.


 213084 1999 TN169                    
        Binzel 2019                    MITHNEOS Method: sVIS


 213471 2002 ES90                     
        Pravec 2019b                   Paired with (80218) 1999 VO123.


 214088 2004 JN13                     
        Warner 2015h                   Period forced to solution derived from 2014 December
                                       observations by Warner.

        Binzel 2019                    MITHNEOS Method: NIR


 214869 2007 PA8                      
        Lin 2018                       Additional observations in 2013 Jan were at much larger phase
                                       angles. Phase reddening may have affected the final result.

        Binzel 2019                    MITHNEOS Method: VISNIR


 214954 2007 WO58                     
        Pravec 2019b                   Paired with (26416) 1999 XM84.


 215188 2000 NM                       
        Binzel 2019                    MITHNEOS Method: TAXON


 216202 2006 UJ13                     
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


 216722 2005 EC286                    
        Binzel 2019                    MITHNEOS Method: sVIS


 217390 2005 CW25                     
        Binzel 2019                    MITHNEOS Method: TAXON


 217796 2000 TO64                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 217807 2000 XK44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 218099 2002 MH3                      
        Pravec 2019b                   Paired with (60744) 2000 GB93.


 218144 2002 RL66                     
        Warner 2010e                   The short period, low amplitude component of the lightcurve
                                       may be due to a widely separated component of a binary that
                                       is a relatively small and irregularly shaped, or a larger but
                                       more regularly shaped body.   If a binary, the period of the
                                       orbit cannot be determined from the observations but is
                                       probably long based on the absence of mutual events and
                                       asynchronous rotation of the two components.  The
                                       low-amplitude component of the lightcurve is U = 1/1+. This
                                       applies not only to the quality of the solution for the
                                       component but to the probability of the asteroid being binary
                                       as well.

        Warner 2010m                   The assignment of primary and secondary in this system is
                                       arbitrary.


 218863 2006 WO127                    
        Binzel 2019                    MITHNEOS Method: NIR


 219071 1997 US9                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 219523 2001 QS84                     
        Binzel 2019                    MITHNEOS Method: sVIS


 220124 2002 TE66                     
        Binzel 2019                    MITHNEOS Method: NIR


 221867 2008 GR90                     
        Pravec 2019b                   Paired with (38184) 1999 KF.


 222165 2000 AX93                     
        Binzel 2019                    MITHNEOS Method: VIS


 224857 2006 YE45                     
        Pravec 2019b                   Paired with (74096) 1998 QD115.


 226268 2003 AN55                     
        Pravec 2019b                   Paired with (409156) 2003 UW156.


 228368 2000 WK10                     
        Binzel 2019                    MITHNEOS Method: VIS


 229007 2003 XF11                     
        Binzel 2019                    MITHNEOS Method: NIR


 229056 2004 FC126                    
        Pravec 2019b                   Paired with (17198) Gorjup.


 229401 2005 SU152                    
        Pravec 2019b                   Paired with 2004 UY97.


 229762 G||'homdima                   
        Grundy 2019a                   Effective diameter for primary body. Satellite diameter: 142
                                       Ãƒâ€šÃ‚Â± 8 km.


 230111 2001 BE10                     
        Binzel 2019                    MITHNEOS Method: NIR


 230979 2005 AT42                     
        Binzel 2019                    MITHNEOS Method: NIR


 231134 2005 TU45                     
        Binzel 2019                    MITHNEOS Method: NIR


 231937 2001 FO32                     
        Binzel 2019                    MITHNEOS Method: NIR


 232691 2004 AR1                      
        Binzel 2019                    MITHNEOS Method: NIR


 233401 2006 FF39                     
        Pravec 2019b                   Paired with (180856) 2005 HX5.


 234061 1999 HE1                      
        Binzel 2019                    MITHNEOS Method: NIR


 234145 2000 EW70                     
        Binzel 2019                    MITHNEOS Method: TAXON


 235756 2004 VC                       
        Binzel 2019                    MITHNEOS Method: NIR


 236716 2007 FV42                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 237442 1999 TA10                     
        Binzel 2019                    MITHNEOS Method: NIR


 238063 2003 EG                       
        Binzel 2019                    MITHNEOS Method: VIS


 241662 2000 KO44                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 241676 2000 QW158                    
        Binzel 2019                    MITHNEOS Method: NIR


 242187 2003 KR18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 242643 2005 NZ6                      
        Binzel 2019                    MITHNEOS Method: NIR


 243025 2006 UM216                    
        Warner 2020c                   A secondary period could not be found.


 244977 2004 BE68                     
        Binzel 2019                    MITHNEOS Method: NIR


 247517 2002 QY6                      
        Binzel 2019                    MITHNEOS Method: NIR


 248083 2004 QU24                     
        Binzel 2019                    MITHNEOS Method: NIR


 248818 2006 SZ217                    
        Binzel 2019                    MITHNEOS Method: NIR


 250112 2002 KY14                     
        Also designated 2007 UL126.


 250322 2003 SC7                      
        Pravec 2019b                   Paired with (52852) 1998 RB75.


 251346 2007 SJ                       
        Binzel 2019                    MITHNEOS Method: NIR


 252399 2001 TX44                     
        Binzel 2019                    MITHNEOS Method: NIR


 252793 2002 FW5                      
        Warner 2017i                   Suspected very wide binary.

        Binzel 2019                    MITHNEOS Method: NIR


 253062 2002 TC70                     
        Binzel 2019                    MITHNEOS Method: VIS


 253841 2003 YG118                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 256412 2007 BT2                      
        Binzel 2019                    MITHNEOS Method: NIR


 257744 2000 AD205                    
        Binzel 2019                    MITHNEOS Method: NIR


 257838 2000 JQ66                     
        Binzel 2019                    MITHNEOS Method: VIS


 258640 2002 ER36                     
        Pravec 2019b                   Paired with (1741) Giclas.


 259585 2003 UG220                    
        Pravec 2019b                   Paired with (122173) 2000 KC28.


 260141 2004 QT24                     
        Binzel 2019                    MITHNEOS Method: NIR


 261878 2006 GR49                     
        Pravec 2019b                   Paired with (112249) 2002 LM9.


 262623 2006 WY2                      
        Binzel 2019                    MITHNEOS Method: NIR


 263976 2009 KD5                      
        Binzel 2019                    MITHNEOS Method: TAXON


 264308 1999 NA5                      
        Binzel 2019                    MITHNEOS Method: NIR


 264357 2000 AZ93                     
        Binzel 2019                    MITHNEOS Method: NIR


 265187 2003 YS117                    
        Binzel 2019                    MITHNEOS Method: NIR


 267182 2000 QX57                     
        Popescu 2018b                  The original Popescu group/family was not used. Instead, one
                                       of the LCDB defaults was used based on the orbital elements


 267494 2002 JB9                      
        Binzel 2019                    MITHNEOS Method: sVISNIR


 267729 2003 FC5                      
        Binzel 2019                    MITHNEOS Method: NIR


 269690 1996 RG3                      
        Binzel 2019                    MITHNEOS Method: NIR


 274138 2008 FU6                      
        Binzel 2019                    MITHNEOS Method: NIR


 274855 2009 RB4                      
        Binzel 2019                    MITHNEOS Method: NIR


 275677 2000 RS11                     
        Warner 2014i                   This entry is for the combined plot from 2014 March 16 and
                                       17.

        Binzel 2019                    MITHNEOS Method: VIS


 275792 2001 QH142                    
        Binzel 2019                    MITHNEOS Method: NIR


 276049 2002 CE26                     
        Warner 2015g                   Using either P1 = 3.088 or 3.298 (found by Pravec et al.,
                                       2006) produces the same period and lightcurve for P2.

        Binzel 2019                    MITHNEOS Method: NIR


 276353 2002 UY20                     
        Pravec 2019b                   Paired with (57202) 2001 QJ53.


 276397 2002 XA40                     
        Binzel 2019                    MITHNEOS Method: NIR


 276400 2002 XS45                     
        Binzel 2019                    MITHNEOS Method: TAXON


 276741 2004 EM66                     
        Binzel 2019                    MITHNEOS Method: NIR


 276770 2004 HC                       
        Binzel 2019                    MITHNEOS Method: NIR


 277127 2005 GW119                    
        Binzel 2019                    MITHNEOS Method: NIR


 277475 2005 WK4                      
        Binzel 2019                    MITHNEOS Method: NIR


 278067 2006 YY40                     
        Pravec 2019b                   Paired with (19289) 1996 HY12.


 279230 2009 UX122                    
        Pravec 2019b                   Paired with (97805) 2000 OJ15.


 279744 1998 KM3                      
        Binzel 2019                    MITHNEOS Method: NIR


 279865 2001 HU24                     
        Pravec 2019b                   Paired with (52773) 1998 QU12.


 282206 2001 VN61                     
        Pravec 2019b                   Paired with (165389) 2000 WC188.


 283319 1992 WR4                      
        Binzel 2019                    MITHNEOS Method: NIR


 283377 2000 PO9                      
        Binzel 2019                    MITHNEOS Method: NIR


 283457 2001 MQ3                      
        Binzel 2019                    MITHNEOS Method: NIR


 283460 2001 PD1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 283827 2003 TP15                     
        Binzel 2019                    MITHNEOS Method: sVIS


 285263 1998 QE2                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 285540 2000 GU127                    
        Binzel 2019                    MITHNEOS Method: VIS


 285631 2000 RB84                     
        Binzel 2019                    MITHNEOS Method: sVIS


 285637 2000 SS4                      
        Pravec 2019b                   Paired with (84203) 2002 RD1333.


 285838 2001 FA1                      
        Binzel 2019                    MITHNEOS Method: NIR


 289315 2005 AN26                     
        Binzel 2019                    MITHNEOS Method: NIR


 291188 2006 AL54                     
        Pravec 2019b                   Paired with (15107) Toepperwein.


 293667 2007 PD19                     
        Pravec 2019b                   Paired with (59184) 1999 AR15.


 295745 2008 UH98                     
        Pravec 2019b                   Paired with (44620) 1999 RS43.


 297274 1996 SK                       
        Binzel 2019                    MITHNEOS Method: NIR


 297418 2000 SP43                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 301844 1990 UA                       
        Binzel 2019                    MITHNEOS Method: NIR


 301964 2000 EJ37                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 302311 2002 AA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 302831 2003 FH                       
        Binzel 2019                    MITHNEOS Method: NIR


 303174 2004 FH11                     
        Binzel 2019                    MITHNEOS Method: sVISNIR


 303712 2005 PR21                     
        Noll 2008d                     No lightcurve observations per se. Two components separated
                                       by 0'.123 ± 0'.009, or about 4000 km. Secondary component
                                       about 1.1 mag fainter than primary.


 305693 2009 BB131                    
        Pravec 2019b                   Paired with (55764) 1992 DG12.


 306376 1983 TA                       
        Binzel 2019                    MITHNEOS Method: NIR


 306453 1999 BE8                      
        Binzel 2019                    MITHNEOS Method: NIR


 306459 1999 GS3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 306895 2001 TT127                    
        Binzel 2019                    MITHNEOS Method: NIR


 307005 2001 XP1                      
        Binzel 2019                    MITHNEOS Method: NIR


 307070 2002 AV31                     
        Binzel 2019                    MITHNEOS Method: NIR


 307161 2002 DY3                      
        Binzel 2019                    MITHNEOS Method: VIS


 307556 2003 EQ43                     
        Binzel 2019                    MITHNEOS Method: sVIS


 307566 2003 FK22                     
        Binzel 2019                    MITHNEOS Method: NIR


 308020 2004 RM222                    
        Binzel 2019                    MITHNEOS Method: sVIS


 308127 2004 XM130                    
        This note applies to all entries for Masiero et al. (2021; Plan. Sci. J. 2, A162). The
        albedo error is the listed maximum possible value when converting albedo values from log
        space to value space. The phase angle in the details record is from the file since the
        actual date of observation was not given. The value for H is the 'model-out' value, which
        may differ slightly from the value used in the NEATM modeling (the value given in Tables
        1-4). This maintains full agreement with the listed albedo and diameter. No specific errors
        for H and G were given. Default values of H_err = 0.05 and G_err = 0.1 were used.


 308635 2005 YU55                     
        Bodewits 2011                  H_V was derived from UV observations that gave H_UV = 25.6.

        Merline 2012                   a = 337 ± 14 m; b = 326 ± 8 m; c = 263 ± 12 m.

        Binzel 2019                    MITHNEOS Method: VISNIR


 309214 2007 LL                       
        Binzel 2019                    MITHNEOS Method: NIR


 309662 2008 EE                       
        Binzel 2019                    MITHNEOS Method: NIR


 310226 2011 SU230                    
        Masiero 2009                   Also identified as 2005 ED209 during the TALCS survey.


 310402 1999 EE5                      
        Binzel 2019                    MITHNEOS Method: VIS


 310429 1999 XP19                     
        Binzel 2019                    MITHNEOS Method: sVIS


 310442 2000 CH59                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 310560 2001 QL142                    
        Pravec 2019web                 Attenuations seen but a consistent secondary period could not
                                       be found.


 311066 2004 DC                       
        Taylor 2006                    Ds ~ 0.060 km.


 311925 2007 BF72                     
        Binzel 2019                    MITHNEOS Method: VIS


 312473 2008 SX245                    
        Binzel 2019                    MITHNEOS Method: sVISNIR


 312497 2009 BR60                     
        Pravec 2019b                   Paired with (3749) Balam.


 313538 2002 YB12                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 313591 2003 MB7                      
        Binzel 2019                    MITHNEOS Method: NIR


 313701 2003 UN3                      
        Pravec 2019b                   Paired with 2012 KL9.


 316651 1990 OL                       
        Binzel 2019                    MITHNEOS Method: sVIS


 316720 1998 BE7                      
        Binzel 2019                    MITHNEOS Method: NIR


 316876 2000 RF43                     
        Binzel 2019                    MITHNEOS Method: sVIS


 316934 2001 AA52                     
        Binzel 2019                    MITHNEOS Method: NIR


 320378 2007 UR3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 321651 2010 BY9                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 322386 2011 QY34                     
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 322652 1999 JO8                      
        Binzel 2019                    MITHNEOS Method: VIS


 322672 1999 TE221                    
        Pravec 2019b                   Paired with (51609) 2001 HZ32.


 322775 2001 HA8                      
        Binzel 2019                    MITHNEOS Method: VIS


 323879 2005 SA204                    
        Pravec 2019b                   Paired with (46162) 2001 FM78.


 325769 2010 LY63                     
        Binzel 2019                    MITHNEOS Method: NIR


 326290 Akhenaten                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 326350 2000 SS217                    
        Binzel 2019                    MITHNEOS Method: sVIS


 326732 2003 HB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 326894 2003 WV25                     
        Pravec 2019b                   Paired with (51866) 2001 PH3.


 329291 2000 JB6                      
        Binzel 2019                    MITHNEOS Method: NIR


 329338 2001 JW2                      
        Binzel 2019                    MITHNEOS Method: NIR


 329437 2002 OA22                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 329520 2002 SV                       
        Binzel 2019                    MITHNEOS Method: NIR


 329614 2003 KU2                      
        Binzel 2019                    MITHNEOS Method: NIR


 330825 2008 XE3                      
        Binzel 2019                    MITHNEOS Method: NIR


 331471 1984 QY1                      
        Warner 2016k                   P2 is not unique (Petr Pravec); it is not possible to
                                       attribute P1 specifically to the period of rotation and P2 to
                                       that of precession.


 331933 2004 TV14                     
        Pravec 2019b                   Paired with (63440) 2001 MD30.


 332446 2008 AF4                      
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2021h                   The results for this record are based on combining
                                       lightcurves from 2021 Jan 9-11. Additional records given the
                                       results using the data from only one of those nights.


 332685 2009 HH36                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 333358 2001 WN1                      
        Binzel 2019                    MITHNEOS Method: NIR


 334527 2002 RG189                    
        Binzel 2019                    MITHNEOS Method: sVIS


 334916 2003 YK39                     
        Pravec 2019b                   Paired with (21436) Chaoyichi.


 337066 1998 BM10                     
        Binzel 2019                    MITHNEOS Method: VIS


 337075 1998 QC1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 337181 1999 VA117                    
        Pravec 2019b                   Paired with (88259) 2001 HJ7.


 337866 2001 WL15                     
        Binzel 2019                    MITHNEOS Method: VIS


 338049 2002 NY31                     
        Binzel 2019                    MITHNEOS Method: VIS


 338176 2002 RC118                    
        Binzel 2019                    MITHNEOS Method: NIR


 339492 2005 GQ21                     
        Binzel 2019                    MITHNEOS Method: NIR


 340211 2006 AR61                     
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


 341520 Mors-Somnus                   
        Sheppard 2011                  R_orbit = 21000 ± 160 km.

        Sheppard 2012a                 Color index: g-i 1.49 ± 0.01. Delta mag between two object:
                                       0.1 mag. Orbital parameters: a = 21000 ± 160 km; e = 0.1529 M
                                       0.0028.


 341843 2008 EV5                      
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.

        Binzel 2019                    MITHNEOS Method: VISNIR


 342842 2008 YB3                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 343098 2009 DV42                     
        Binzel 2019                    MITHNEOS Method: NIR


 344074 1997 UH9                      
        Binzel 2019                    MITHNEOS Method: VIS


 344143 2000 JQ3                      
        Binzel 2019                    MITHNEOS Method: sVIS


 345705 2006 VB14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 345853 2007 PU11                     
        Binzel 2019                    MITHNEOS Method: NIR


 347813 2002 NP1                      
        Binzel 2019                    MITHNEOS Method: NIR


 348018 2003 SF334                    
        Pravec 2019b                   Paired with (9783) Tensho-kan.


 348400 2005 JF21                     
        Period for first entry from Oey 2016b (Date = 09/24/2015) is for the combined data set
        covering five months. Subsequent listings are for subsets within the overall span.

        Naidu 2015c                    Possible indications of a second satellite. No period for
                                       primary or orbital period of first satellite given.


 348452 2005 RU20                     
        Pravec 2019b                   Paired with (418312) 2008 FF88.


 349068 2006 YT13                     
        Binzel 2019                    MITHNEOS Method: NIR


 350513 2000 BG19                     
        Binzel 2019                    MITHNEOS Method: VIS


 350523 2000 EA14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 350716 2001 XO105                    
        Pravec 2019b                   Paired with (4765) Wasserburg.


 350751 2002 AW                       
        Pravec 2022a                   SR-SZ = 0.12 Â± 0.05


 350988 2003 GW                       
        Binzel 2019                    MITHNEOS Method: NIR


 351549 2005 TJ73                     
        Binzel 2019                    MITHNEOS Method: sVIS


 352143 2007 LR32                     
        Binzel 2019                    MITHNEOS Method: NIR


 353866 2012 WN2                      
        The designation of 2006 SU210 originally assigned to this object was updated. The MPC has
        since designated this as (353866) 2012 WN2.


 353938 1998 QR15                     
        Binzel 2019                    MITHNEOS Method: VIS


 354030 2001 RB18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 354127 2002 BP26                     
        Binzel 2019                    MITHNEOS Method: VIS


 354182 2002 DU3                      
        Binzel 2019                    MITHNEOS Method: VIS


 354652 2005 JY103                    
        Pravec 2019b                   Paired with (76111) 2000 DK106.


 354952 2006 FJ9                      
        Binzel 2019                    MITHNEOS Method: NIR


 356991 1998 QA1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 357022 1999 YG3                      
        Binzel 2019                    MITHNEOS Method: VIS


 357152 2002 CO15                     
        Binzel 2019                    MITHNEOS Method: NIR


 357439 2004 BL86                     
        Radar Team 2015a               D_primary: 0.325 km. D_satellite: 0.070 km. Discovey credit
                                       goes to Pollock et al.


 357618 2005 EM30                     
        Binzel 2019                    MITHNEOS Method: NIR


 359592 2010 VA1                      
        Binzel 2019                    MITHNEOS Method: NIR


 359995 2012 VA102                    
        The original designation was 2006 SW275. This is now identified by the MPC as 2012 VA102.

        Masiero 2009                   The original designation was 2006 SW275. This is now
                                       identified by the MPC as 2012 VA102.


 360191 1988 TA                       
        Binzel 2019                    MITHNEOS Method: NIR


 360433 2002 JR9                      
        Binzel 2019                    MITHNEOS Method: NIR


 361071 2006 AO4                      
        Binzel 2019                    MITHNEOS Method: NIR


 362310 2009 UM3                      
        Binzel 2019                    MITHNEOS Method: NIR


 363067 2000 CO101                    
        Taylor 2009                    Estimated sizes: P = 0.525 km; S = 0.045 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


 363075 2000 OG8                      
        Binzel 2019                    MITHNEOS Method: NIR


 363305 2002 NV16                     
        Binzel 2019                    MITHNEOS Method: VIS


 363505 2003 UC20                     
        Binzel 2019                    MITHNEOS Method: NIR


 363599 2004 FG11                     
        Binzel 2019                    MITHNEOS Method: TAXON


 363790 2005 JE46                     
        Binzel 2019                    MITHNEOS Method: NIR


 363814 2005 ND7                      
        Binzel 2019                    MITHNEOS Method: NIR


 364171 2006 JZ81                     
        Parker 2011                    Satellite obrital period: 4.11 ± 0.15 years.


 365071 2009 AV                       
        Binzel 2019                    MITHNEOS Method: NIR


 365246 2009 NE                       
        Binzel 2019                    MITHNEOS Method: TAXON


 365424 2010 KX7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 366774 2004 TB18                     
        Binzel 2019                    MITHNEOS Method: TAXON


 366833 2005 MC                       
        Binzel 2019                    MITHNEOS Method: NIR


 367248 2007 MK13                     
        Binzel 2019                    MITHNEOS Method: NIR


 367251 2007 PN49                     
        Binzel 2019                    MITHNEOS Method: NIR


 367922 2012 BG133                    
        Pravec 2019b                   Paired with (453106) 2007 WR62.


 367943 Duende                        
        Gary 2013a                     H, D, and pV assume a type S asteroid. A type V was also
                                       considered possible from spectrophotometric observations.

        Binzel 2019                    MITHNEOS Method: VIS

        Moskovitz 2020                 Period is post-flyby. Analysis indicates pre-flyby period of
                                       8.4 h.


 368313 2002 PY103                    
        Pravec 2019b                   Paired with (101065) 1998 RV11.


 368664 2005 JA22                     
        Binzel 2019                    MITHNEOS Method: NIR


 370037 2000 SV20                     
        Binzel 2019                    MITHNEOS Method: NIR


 370061 2000 YO29                     
        Binzel 2019                    MITHNEOS Method: VIS


 370866 2005 EB37                     
        Binzel 2019                    MITHNEOS Method: sVIS


 371660 2007 CN26                     
        Binzel 2019                    MITHNEOS Method: NIR


 374158 2004 UL                       
        Warner 2015h                   Period is a best-fit single period.


 374851 2006 VV2                      
        Binzel 2019                    MITHNEOS Method: NIR


 374855 2006 VQ13                     
        Binzel 2019                    MITHNEOS Method: NIR


 375103 2007 TD71                     
        Binzel 2019                    MITHNEOS Method: NIR


 376169 2011 BH162                    
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 376713 1995 WQ5                      
        Binzel 2019                    MITHNEOS Method: VIS


 376848 2001 RY47                     
        Binzel 2019                    MITHNEOS Method: NIR


 377732 2005 XJ8                      
        Warner 2022j                   Suspect 'wide binary'.


 380188 2000 WC67                     
        Binzel 2019                    MITHNEOS Method: VIS


 380929 2006 HU30                     
        Binzel 2019                    MITHNEOS Method: NIR


 381906 2010 CL19                     
        Binzel 2019                    MITHNEOS Method: NIR


 382758 2003 GY                       
        Binzel 2019                    MITHNEOS Method: VIS


 385186 1994 AW1                      
        Binzel 2019                    MITHNEOS Method: VIS


 385203 1999 SO15                     
        Binzel 2019                    MITHNEOS Method: TAXON


 385343 2002 LV                       
        Binzel 2019                    MITHNEOS Method: NIR


 385446 Manwe                         
        Grundy 2014                    Color indexes are for primary. The satellite showed about
                                       Ãƒâ€šÃ‚Â± 0.15 mag difference, or essentially the same color.
                                       Spin axis is for orbital pole with the primary pole presumed
                                       to be the same or very similar.

        Rabinowitz 2020                Period/amplitude are for combined system. Albedo is for
                                       primary. Orbital period for satellite is based on monomodal
                                       lightcurve.


 386298 2008 SR7                      
        Binzel 2019                    MITHNEOS Method: NIR


 388838 2008 EZ5                      
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2019web                 Suspected, low amplitude secondary period: nature
                                       undetermined.


 391151 2005 YY93                     
        Binzel 2019                    MITHNEOS Method: NIR


 393274 2013 WJ82                     
        Pravec 2019b                   Paired with (63047) 2000 WQ93.


 393359 1998 ME3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 394066 2005 XU77                     
        Binzel 2019                    MITHNEOS Method: NIR


 394130 2006 HY51                     
        Binzel 2019                    MITHNEOS Method: NIR


 396593 2001 HC                       
        Binzel 2019                    MITHNEOS Method: NIR


 398188 Agni                          
        Warner 2023a                   Final soultion required P3 = 9.48 h, A3 = 0.23 mag. P2 and P3
                                       are probably artifacts of using additive multi-period
                                       analysis on a tumbler.


 399307 1991 RJ2                      
        Binzel 2019                    MITHNEOS Method: NIR


 399418 2001 VD77                     
        Binzel 2019                    MITHNEOS Method: sVIS


 399433 2001 YK4                      
        Binzel 2019                    MITHNEOS Method: VIS


 399497 2002 TV190                    
        Masiero 2009                   Maisero et al. identified TALCS 126 as 2006 SZ2. This is a
                                       newer designation for 2002 TV190, which is the one included
                                       in the MPCORB file.


 399774 2005 NB7                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 401857 2000 PG3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 402267 2005 QE166                    
        Binzel 2019                    MITHNEOS Method: NIR


 403049 2008 AY36                     
        Binzel 2019                    MITHNEOS Method: NIR


 405058 2001 TX16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 407656 2011 SL102                    
        Binzel 2019                    MITHNEOS Method: NIR


 408792 2000 GF2                      
        Binzel 2019                    MITHNEOS Method: NIR


 409156 2003 UW156                    
        Pravec 2019b                   Paired with (226268) 2003 AN55.


 409204 2003 WX25                     
        Binzel 2019                    MITHNEOS Method: NIR


 409995 2006 WV3                      
        Binzel 2019                    MITHNEOS Method: NIR


 410195 2007 RT147                    
        Binzel 2019                    MITHNEOS Method: NIR


 410627 2008 RG1                      
        Binzel 2019                    MITHNEOS Method: NIR


 410650 2008 SQ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 410778 2009 FG19                     
        Binzel 2019                    MITHNEOS Method: NIR


 411280 2010 SL13                     
        Binzel 2019                    MITHNEOS Method: NIR


 412065 2013 ET86                     
        Pravec 2019b                   Paired with (11677) 1998 DY4.


 412976 1987 WC                       
        Binzel 2019                    MITHNEOS Method: NIR


 413038 2001 MF1                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 413123 2001 XS1                      
        Binzel 2019                    MITHNEOS Method: VIS


 413563 2005 TG45                     
        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       90.5-64.4 deg. The H_SR values are the linear extrapolation
                                       using the phase slope (beta_SR) of 0.03259. The lack of low
                                       phase angles prevented use of H-G or HG1,G2 modeling.


 413577 2005 UL5                      
        Pravec 2015web                 Secondary period might be due to being binary.

        Binzel 2019                    MITHNEOS Method: NIR


 414166 2008 AU67                     
        Pravec 2019b                   Paired with (56700) 2000 LL28.


 414287 2008 OB9                      
        Binzel 2019                    MITHNEOS Method: NIR


 414586 2009 UV18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 414990 2011 EM51                     
        Binzel 2019                    MITHNEOS Method: NIR


 415711 1998 WT7                      
        Binzel 2019                    MITHNEOS Method: NIR


 415949 2001 XY10                     
        Binzel 2019                    MITHNEOS Method: VIS


 415992 2002 AT49                     
        Pravec 2019b                   Paired with (87887) 2000 SS286.


 416151 2002 RQ25                     
        Binzel 2019                    MITHNEOS Method: NIR


 416186 2002 TD60                     
        Warner 2015r                   Period analysis by Pravec (Czech Institute).

        Binzel 2019                    MITHNEOS Method: VISNIR


 416195 2002 TR190                    
        Binzel 2019                    MITHNEOS Method: NIR


 416231 2003 AJ73                     
        Binzel 2019                    MITHNEOS Method: NIR


 416591 2004 LC2                      
        Binzel 2019                    MITHNEOS Method: TAXON


 416680 2004 XD50                     
        Binzel 2019                    MITHNEOS Method: TAXON


 416694 2004 YR32                     
        Warner 2021g                   Suspected very wide binary, which would make the 50-h period
                                       that of the primary's rotatation, not the orbital period of
                                       the satellite.


 418312 2008 FF88                     
        Pravec 2019b                   Paired with (348452) 2005 RU20.


 418797 2008 VF                       
        Binzel 2019                    MITHNEOS Method: NIR


 419464 2010 CC180                    
        Binzel 2019                    MITHNEOS Method: NIR


 420187 2011 GA55                     
        Binzel 2019                    MITHNEOS Method: NIR


 420738 2012 TS                       
        Binzel 2019                    MITHNEOS Method: NIR


 421781 2014 QG22                     
        Pravec 2019b                   Paired with (53576) 2000 CS47.


 422686 2000 AC6                      
        Binzel 2019                    MITHNEOS Method: VIS


 423321 2005 ED318                    
        Binzel 2019                    MITHNEOS Method: NIR


 428086 2006 NM                       
        Binzel 2019                    MITHNEOS Method: NIR


 430439 2000 LF6                      
        Binzel 2019                    MITHNEOS Method: TAXON


 430484 2001 ST246                    
        Chang (2015) H values are based on H-G system. The G values are in R, not V. All lightcurves
        with a period were given U = 2 regardless of rating by Chang et al.


 430804 2005 AD13                     
        Binzel 2019                    MITHNEOS Method: NIR


 433939 1995 DW1                      
        Binzel 2019                    MITHNEOS Method: NIR


 433953 1997 XR2                      
        Pravec 2019web                 Second period in tumbling solution is not unique.


 434096 2002 GO5                      
        Binzel 2019                    MITHNEOS Method: NIR


 436459 2011 CL97                     
        Pravec 2019b                   Paired with (49791) 1999 XF31.


 436551 2011 GD83                     
        Pravec 2019b                   Paired with (16815) 1997 UA9.


 437841 1998 HD14                     
        Binzel 2019                    MITHNEOS Method: TAXON


 437844 1999 MN                       
        Binzel 2019                    MITHNEOS Method: TAXON


 437905 2001 XU30                     
        Binzel 2019                    MITHNEOS Method: VIS


 438105 2005 GO22                     
        Binzel 2019                    MITHNEOS Method: NIR


 440212 2004 OB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 441549 2008 TM68                     
        Pravec 2019b                   Paired with (43008) 1999 UD31.


 442523 2011 WU95                     
        Binzel 2019                    MITHNEOS Method: NIR


 443103 2013 WT67                     
        Warner 2015c                   Period is estimate for one of the two tumbling periods.


 443837 2000 TJ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 445775 2011 YA                       
        Binzel 2019                    MITHNEOS Method: NIR


 446085 2013 CW179                    
        Pravec 2019b                   Paired with (66659) 1999 TJ1.


 446791 1998 SJ70                     
        Binzel 2019                    MITHNEOS Method: NIR


 446804 1999 VN6                      
        Binzel 2019                    MITHNEOS Method: VIS


 448003 2008 DE                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 448972 2011 YV15                     
        Binzel 2019                    MITHNEOS Method: NIR


 450293 2004 LV3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 450894 2008 BT18                     
        Benner 2008a                   Arecibo and Goldstone observations show: D1: 0.6 km D2: >0.2
                                       km Sep: 1.5 km.

        Warner 2018h                   No sign of primary rotatin of about 2.5 h.

        Binzel 2019                    MITHNEOS Method: NIR


 451124 2009 KC3                      
        Binzel 2019                    MITHNEOS Method: NIR


 451157 2009 SQ104                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 451397 2011 EZ78                     
        Pravec 2011web                 Two suspect attentuations were seen but not confirmed.

        Skiff 2011web                  Data suggests possibility of tumbling or binary.

        Binzel 2019                    MITHNEOS Method: VISNIR


 452334 2001 LB                       
        Binzel 2019                    MITHNEOS Method: NIR


 452389 2002 NW16                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 452561 2005 AB                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 452773 2006 DM14                     
        Binzel 2019                    MITHNEOS Method: sVIS


 452807 2006 KV89                     
        Binzel 2019                    MITHNEOS Method: NIR


 453106 2007 WR62                     
        Pravec 2019b                   Paired with (367922) 2012 BG133.


 453563 2010 BB                       
        Binzel 2019                    MITHNEOS Method: NIR


 453818 2011 SJ109                    
        Pravec 2019b                   Paired with (25021) Nischaykumar.


 455157 1997 YM3                      
        Binzel 2019                    MITHNEOS Method: TAXON


 455185 2000 EB107                    
        Binzel 2019                    MITHNEOS Method: TAXON


 455192 2000 QN130                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 455213 2001 OE84                     
        Binzel 2019                    MITHNEOS Method: VIS


 455322 2002 NX18                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 455327 2002 OP28                     
        Pravec 2019b                   Paired with (9068) 1993 OD.


 455415 2003 GA                       
        Binzel 2019                    MITHNEOS Method: VISNIR


 455426 2003 MT9                      
        Binzel 2019                    MITHNEOS Method: NIR


 455578 2004 RA216                    
        Binzel 2019                    MITHNEOS Method: sVIS


 455594 2004 SV55                     
        Binzel 2019                    MITHNEOS Method: TAXON


 456301 2006 SV134                    
        Binzel 2019                    MITHNEOS Method: NIR


 459200 2012 DK61                     
        Binzel 2019                    MITHNEOS Method: NIR


 461501 2003 FT3                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 461852 2006 GY2                      
        Benner 2006b                   Secondary diameter estimated to be 0.08 km and orbital
                                       separation at least 0.5 km.


 461912 2006 RG2                      
        Binzel 2019                    MITHNEOS Method: NIR


 462176 2007 TC334                    
        Pravec 2019b                   Paired with (70511) 1999 TL103.


 464797 2004 FZ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 464798 2004 JX20                     
        Skiff 2019web                  The solutions are not unique.


 464815 2004 RV257                    
        Binzel 2019                    MITHNEOS Method: sVIS


 465402 2008 HW1                      
        Binzel 2019                    MITHNEOS Method: NIR


 465616 2009 EC                       
        Warner 2016m                   Suspected very wide binary.


 467317 2000 QW7                      
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2020c                   Two possibilities: single period with large zero-point
                                       offsets or tumbling with near zero offsets.


 467336 2002 LT38                     
        Warner 2023f                   P1 is dominant, though it may still be a multiple of the true
                                       frequency (1/P1). P2 is one of several solutions but it is
                                       the one that gave the best fit when subtracting from the raw
                                       data.


 467460 2006 JF42                     
        Binzel 2019                    MITHNEOS Method: NIR

        Pravec 2022web                 Alternate solutions ampltides assumed to be the same as the
                                       adopted period.


 468738 2010 TN54                     
        Binzel 2019                    MITHNEOS Method: NIR


 469438 2002 GV31                     
        Pal 2015b                      V-R assumed.


 469446 2002 NL8                      
        Binzel 2019                    MITHNEOS Method: sVIS


 469513 2003 QR79                     
        Binzel 2019                    MITHNEOS Method: VIS


 469896 2005 WC1                      
        Miles 2008b                    Given period based on 3 nights (Miles, private
                                       communications). JBAA publication gives period of 2.57 h base
                                       on one night.


 470004 2006 MJ10                     
        Binzel 2019                    MITHNEOS Method: NIR


 470975 2009 SC15                     
        Binzel 2019                    MITHNEOS Method: VIS


 471240 2011 BT15                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 474158 1999 FA                       
        Binzel 2019                    MITHNEOS Method: VIS


 474370 2002 RT157                    
        Binzel 2019                    MITHNEOS Method: sVIS


 475665 2006 VY13                     
        Binzel 2019                    MITHNEOS Method: NIR

        Warner 2022j                   Secondary period is almost 3:1 with dominant period and may
                                       be a harmonic artifcat of the analysis.


 477465 2009 XZ1                      
        Binzel 2019                    MITHNEOS Method: NIR


 477762 2010 XZ67                     
        Binzel 2019                    MITHNEOS Method: NIR


 479358 2013 XN8                      
        Pravec 2019b                   Asteroid pair with 5478 Wartburg.


 480820 1998 VF32                     
        Binzel 2019                    MITHNEOS Method: NIR


 480858 2001 PT9                      
        Binzel 2019                    MITHNEOS Method: NIR


 480883 2001 YE4                      
        Binzel 2019                    MITHNEOS Method: VISNIR


 481032 2004 YZ23                     
        Binzel 2019                    MITHNEOS Method: NIR


 481085 2005 SA135                    
        Pravec 2019b                   Paired with (21028) 1989 TO.


 481090 2005 SY173                    
        Binzel 2019                    MITHNEOS Method: sVIS


 481532 2007 LE                       
        Brozovic 2012                  Estimated sizes: Dp 0.5 km; Ds 0.18 km. Orbital separation >
                                       0.8 km.

        Binzel 2019                    MITHNEOS Method: VISNIR


 481542 2007 RF5                      
        Binzel 2019                    MITHNEOS Method: NIR


 482250 2011 LL2                      
        Pravec 2022web                 Seconary solution amplitude assumed to be the same as the
                                       primary amplitude.


 482796 2013 QJ10                     
        Binzel 2019                    MITHNEOS Method: NIR


 483422 2000 CE59                     
        Binzel 2019                    MITHNEOS Method: VIS


 483423 2000 DO1                      
        Binzel 2019                    MITHNEOS Method: VIS


 484757 2009 BL2                      
        Binzel 2019                    MITHNEOS Method: NIR


 484976 2009 UN3                      
        Binzel 2019                    MITHNEOS Method: NIR


 485051 2010 CM44                     
        Binzel 2019                    MITHNEOS Method: NIR


 486958 Arrokoth                      
        Porter 2019                    Diamter is volume of equivalent sphere based on the overall
                                       dimensions of the contact binary system. The individual
                                       volumes are 15.9 km and 12.9 km.

        Stern 2019                     Effective diameter (from volume): Ultima: 13.88 km; Thule:
                                       12.61 km. Phase angle is viewed from Earth.

        Hofgartner 2021                Viewing aspect is from Earth.


 488453 1994 XD                       
        Binzel 2019                    MITHNEOS Method: NIR


 488515 2001 FE90                     
        Binzel 2019                    MITHNEOS Method: TAXON


 489337 2006 UM                       
        Binzel 2019                    MITHNEOS Method: NIR


 492143 2013 OE                       
        Warner 2020c                   A third period was found as well: P3 = 4.88 h.


 495833 2000 SB8                      
        Binzel 2019                    MITHNEOS Method: NIR


 495858 2003 MJ4                      
        Binzel 2019                    MITHNEOS Method: NIR


 496001 2007 VR183                    
        Binzel 2019                    MITHNEOS Method: NIR


 496028 2008 SC9                      
        Pravec 2019b                   Paired with (14806) 1091 EV25.


 496923 2001 UW57                     
        Originally Derm3d in Dermawan Ph.D. thesis.


 497676 2006 SR2                      
        Binzel 2019                    MITHNEOS Method: sVIS


 500080 2011 WV134                    
        Binzel 2019                    MITHNEOS Method: VISNIR


 501710 2014 UY23                     
        Pravec 2019b                   Paired with (88666) 2001 RP79.


 503861 1998 WZ1                      
        Binzel 2019                    MITHNEOS Method: TAXON


 503871 2000 SL                       
        Binzel 2019                    MITHNEOS Method: sVISNIR


 503941 2003 UV11                     
        Binzel 2019                    MITHNEOS Method: NIR


 503955 2004 ED107                    
        Pravec 2019b                   Paired with (53537) 2000 AZ239.


 504025 2005 RQ6                      
        Binzel 2019                    MITHNEOS Method: NIR


 504887 2010 WL                       
        Binzel 2019                    MITHNEOS Method: NIR


 505476 2013 UL15                     
        Alexandersen 2018              Applies to all Alexandersen 2018: For those objects in their
                                       list that were found in MPCOrb, the Hv magnitude was nearly
                                       the same as their Hr (Pan-STARRS r). The original Hr is
                                       reported in the detail record _and_ used for H in the summary
                                       table if an MPCOrb value was not available.


 506437 2000 WL10                     
        Binzel 2019                    MITHNEOS Method: VIS


 506459 2002 AL14                     
        Binzel 2019                    MITHNEOS Method: VISNIR


 508774 1999 JE1                      
        Binzel 2019                    MITHNEOS Method: VIS


 508908 2003 YX1                      
        Binzel 2019                    MITHNEOS Method: VIS


 510132 2010 UY57                     
        Pravec 2019b                   Paired with (6369) 1983 UC.


 514596 2003 FG                       
        Binzel 2019                    MITHNEOS Method: NIR


 516398 2001 HW15                     
        Binzel 2019                    MITHNEOS Method: VIS


 516420 2003 FS2                      
        Binzel 2019                    MITHNEOS Method: VIS


 516435 2004 FJ29                     
        Binzel 2019                    MITHNEOS Method: NIR


 518482 2005 TZ42                     
        Binzel 2019                    MITHNEOS Method: sVIS


 518507 2006 EE1                      
        Binzel 2019                    MITHNEOS Method: NIR


 518810 2010 CF19                     
        Binzel 2019                    MITHNEOS Method: NIR


 523625 2008 DG17                     
        Warner 2018h                   2018 radar observations indicate a period of ~2.8 h, but a
                                       slightly longer period is possible. The photometric data do
                                       not allow formally excluding a solution near 7.3 h.


 523775 2014 YB35                     
        Naidu 2015b                    Ds: < 150 m.


 523806 2002 WW17                     
        Cutri 2019                     The analysis used W1 and W2 NEOWISE data.

        Cutri 2019                     The analysis used W1 and W2 NEOWISE data.


 523855 1995 SK87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html


 523856 1995 SL87                     
        The phase angle and PAB in the details record were computed using the mean JD given in the
        file. H-G are from MPCORB or custom MPC values. See the documentation in the PDS4
        documentation at https://sbn.psi.edu/pds/resource/neowisediam.html

        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 525939 2005 UY97                     
        Pravec 2019b                   Paired with (229401) 2005 SU152.


 528159 2008 HS3                      
        Warner 2019p                   Single period analysis found several dominant periods. They
                                       are listed in the Ambiguous table.


 528407 2008 TO52                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 531119 2012 FF11                     
        Pravec 2019b                   Paired with (69298) 1992 DR9.


 531260 2012 KL9                      
        Pravec 2019b                   Paired with (313701) 2003 UN3.


 532037 2013 FY27                     
        Sheppard 2018c                 Separation from primary about 9800 km.


 537342 2015 KN120                    
        Warner 2018a                   P3/A3: 7.448 ± 0.006, 0.12 ± 0.03 mag. P2 and P3 may be a
                                       single period corrupted by harmonics of P1, or P1 and the
                                       true P2 are tumble frequencies beating to produce a third
                                       apparent frequency.


 541818 2012 AX10                     
        Pravec 2019b                   Paired with (33325) 1998 RH3.


 545135 2014 YE64                     
        Binzel 2019                    MITHNEOS Method: sVIS


 554099 2012 KU50                     
        Chandler 2021                  Binary discovery. Semi-major axis > 15000 km.


 561272 2015 RV228                    
        Pravec 2019b                   Paired with (98866) Giannabussolari.


 575395 2011 SE164                    
        Pravec 2019b                   Paired with (100440) 1996 PJ6.


 576293 2012 LB9                      
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 577283 2013 CT63                     
        Pravec 2019b                   Paired with (63970) 2001 SG72.


 590180 2011 SR158                    
        Pravec 2019b                   Paired with (8306) Shoko.


 606952 2019 WF6                      
        The period is an approximaation of a short-term periood superimpoed on a longer period, or
        the dominant period of a tumbler.


 611007 2006 QN54                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.


 612023 1994 VX3                      
        Mainzer 2019                   The phase angle and PAB in the details record were computed
                                       using the mean JD given in the file. H-G are from MPCORB or
                                       custom MPC values. See the documentation in the PDS4
                                       documentation at
                                       https://sbn.psi.edu/pds/resource/neowisediam.html


 612050 1997 GL3                      
        Skiff 2023                     The given period is for an apparent short-term component of
                                       the overall lightcurve. This may be an artifact or an element
                                       of a tumbler.


 612147 2000 CF105                    
        Parker 2011                    Satellite orbital period: 10.92 ± 0.12 years.


 612242 2001 QQ322                    
        Noll 2008d                     No lightcurve observations per se. Two components of about
                                       equal size separated by 0'.1272 ± 0'.0015, or about 4000 km.
                                       


 612687 2003 UN284                    
        Parker 2011                    Satellite orbital period: 8.73 ± 0.65 years.


 612813 2004 RF84                     
        Benner (2006a) observed with radar and found a dimension of at least 1.2 km based on echo
        delay range. However, the images indicate the possibility of a bifurcated body with an
        effective diameter of about 1.5 km. Based on the total information, we presumed a dark
        (C-type) asteroid and used the default albedo for that class and MPCORB H to derive a
        diameter.


 612929 2005 CR37                     
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


 613512 2006 SK134                    
        Warner 2019m                   The two periods given for this likely tumbler are best-fit
                                       single periods and not formal two-period analysis.


 614473 2009 SZ67                     
        Pravec 2019b                   Paired with (105247) 2000 QH3.


 616600 2006 AN29                     
        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


 620071 2011 WN15                     
        Pravec 2019web                 Possible color variations during rotation.


      0 103P/Hartley                  
        Harmon 2010                    The diameter is based the long-axis dimension of a
                                       highly-elongated, bilobate object as observed by radar. The
                                       radar cross section was 0.04 km^2, which corresponds to a
                                       diameter of ~100 m.


      0 10P/Tempel 2                  
        A'Hearn 1989                   Amplitude is for observations at 4845 Angstroms. Other
                                       amplitudes: 6840 A, 0.45 mag; 10100 A, 0.8 mag.


      0 169P/NEAT                     
        Determined to be a comet (by Warner) after receiving an asteroid designation. Current MPC
        designation is P/2002 EX12.


      0 1994 CJ1                      
        Radar Team 2014b               First estimate is two 100-m bodies about 500-m apart.


      0 1994 ES2                      
        Terai 2018                     Entries for Terai 2017 in the Color Index table were derived
                                       from their Hg-r and Hr-i. The errors were found by adding the
                                       individual errors in quadrature.


      0 1998 WV24                     
        Benecchi 2008                  The two components were separated by an angular distance of
                                       0'.051 ± 0'.002, with the secondary fainter by 0.3 magnitude.
                                       The secondary was located at 0'.033 ± 0'.003 in R.A. and
                                       0'.039 ± 0'.003 in Decl. relative to the primary.


      0 1999 TE21                     
        This note applies to all Erasmus 2019 (2019ApJS..242...15E) detail records: Initial bulk
        data entry assigned U = 2 ONLY if PFlag was empty and pending individual review.

        Erasmus 2019                   This note applies to all Erasmus 2019 (2019ApJS..242...15E)
                                       detail records: Initial bulk data entry assigned U = 2 only
                                       if PFlag was empty and pending individual review. Amplitude
                                       errors were given only when the AmpFlag was empty.


      0 2000 UK11                     
        Nolan 2001                     It appears that Nolan made a factor of 2 error in his
                                       reported period. The LCDB adopts the 0.025 h period based on
                                       the reported observational data of radar bandwidth and
                                       estimated size of 30 meters.


      0 2001 QW322                    
        Parker 2011                    Satellite orbital period: 17.01 ± 1.55 years.


      0 2001 RW17                     
        Warner 2020a                   8-hour solution unlikely but cannot be formally excluded.


      0 2003 QY90                     
        Benecchi 2009                  See note under 2001 QC298.

        Grundy 2011                    Orbital period determined from astrometric measurements.


      0 2005 GQ107                    
        Pravec 2019b                   Paired with (55913) 1998 FL12.


      0 2005 LW3                      
        Naidu 2022                     Primary-Seoncdary distance ~ 4 km.


      0 2005 WW113                    
        Pravec 2019b                   Paired with (5026) Martes.


      0 2006 BR284                    
        Parker 2011                    Satellite orbital period: 4.11 ± 0.04 years.


      0 2006 CH69                     
        Parker 2011                    Satellite orbital period: 3.89 ± 0.07 years.


      0 2006 SF369                    
        Noll 2008b                     No lightcurves per se. Hubble observations show a binary
                                       system of about the same size separated by 0'.109 ± 0'.003,
                                       or about 3200 km.


      0 2007 TQ24                     
        Warner 2020c                   Second period is ambiguous. Alternate solution: P_2B: 9.57 h.


      0 2008 SD                       
        The geocentric phase angle and PAB in the Masiero 2020b details records were computed using
        the mean MJD given in the file. H-G are the values used for the model and appear only in
        details records. The MPCORB H-G at the time of import are used in the summary line. The
        albedo error is the larger linear error listed in the table. The diameter is the corrected
        value (see Masiero et al. 2020b).

        Masiero 2020b                  The geocentric phase angle and PAB in the Masiero 2020b
                                       details records were computed using the mean MJD given in the
                                       file. H-G are the values used for the model and appear only
                                       in details records. The MPCORB H-G at the time of import are
                                       used in the summary line. The albedo error is the larger
                                       linear error listed in the table. The diameter is the
                                       corrected value (see Masiero et al. 2020b).


      0 2008 TC3                      
        Aleshkina 2011                 Periods of 18 m and 6.89 h were also reported. The LCDB
                                       authors believe these to be spurious, possibly because
                                       non-principal axis rotation was not taken into account.


      0 2008 TT26                     
        Ryan 2009                      http://infohost.nmt.edu/~bryan/research/work/mro_images/k08t2
                                       6t/k08t26t_081019.jpg


      0 2008 UZ220                    
        Pravec 2019b                   Paired with (103055) 1999 XR134.


      0 2009 BD                       
        Mommert 2014c                  Diameter and albedo based on a rocky body. An equally likely
                                       solution assuming a collection of bare rock slabs gives D =
                                       0.004 ± 0.001 km and pV = 0.45 ± 0.35.


      0 2009 QZ66                     
        This note applies to all Lo et al. (2020, AJ 159) entries. A suffix of 'Lo21-' has been
        added to the all-numeric internal IDs used by Lo et al. to avoid confusion with an
        MPC-assigned number. The astrometric data they provided was used to match each of their
        objects to one in the MPCOrb data set. In most cases, the cross-match was unambiguous. For
        the others, there will be an entry in the extended notes for that particular Lo et al.
        details record. This is particularly important for objects in the summary line that have
        only the Lo et al. reference and are flagged as uncertain. Here, the object listed may not
        be the correct one. The Date, PAB_L, PAB_B, and Phase entries in the details record are
        based on 1) the cross-matched ID and 2) the first date of observations, which usually
        spanned about three days.


      0 2010 RC130                    
        Skiff 2019b                    Analysis by P. Pravec. A single period of 8.687 h was
                                       initially found, but this is a beat period based on a 3:5
                                       ratio of the periods found with 2-dimensional Fourier
                                       analysis. The periods could be a linear combination of the
                                       two actual periods (precession and rotation).


      0 2010 WC9                      
        Beniyama 2022                  This applies to all Beniyama 2022 entries: the observations
                                       were made with a video camera taking multiple frams per
                                       second.


      0 2011 CT4                      
        Pravec 2020web                 A higher than normal albedo was used to calculate a revised
                                       diameter based on the new H-G values.


      0 2011 FJ54                     
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2011 HP                       
        Warner 2019p                   Period and amplitudes based on full data set.


      0 2011 TG2                      
        Warner 2023a                   Period of combined data set.


      0 2011 UT239                    
        Masiero 2009                   At the time of the TALCS survey, this object had the
                                       desgination of 2006 SP242. The MPCORB file not identifies it
                                       as 2011 UT239.


      0 2011 XA3                      
        Urakawa 2014                   H, D, and pV assume a type S asteroid. A type V was also
                                       considered possible from spectrophotometric observations.


      0 2012 LZ1                      
        Hicks 2012d                    Authors gave period as 5-16 hours. The two periods given are
                                       the approximae values based on their period spectrum from
                                       Fourier analysis.

        Howell 2012b                   The diameter is the approximate effecitve diameter based on a
                                       longest dimension of about 1 km. The albedo is the average of
                                       the range estimated based on H = 19.8.


      0 2012 PG6                      
        Warner 2023a                   Result of 2022 Sep 24+28.

        Warner 2023a                   Result of combined data set.

        Warner 2023a                   Result of 2022 Sep 26+28.

        Warner 2023a                   Result of 2022 Sep 24+26.


      0 2012 TC4                      
        Urakawa 2019                   Period is for precession. NPAR P2 is rotation period.


      0 2012 TK84                     
        Pravec 2019b                   Paired with (167405) 2003 WP118.


      0 2012 TS209                    
        Pravec 2019b                   Paired with (26420) 1999 XL103.


      0 2012 UX136                    
        Pravec 2012web                 Based on data from Joe Pollock.


      0 2014 AC                       
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2014 AN51                     
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2014 CH9                      
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2014 EX61                     
        2016 UV197 may have been the designation at the time. Using the MPC MP Checker, the
        astrometric position from Lo et al. (2020), 2014 EX61 has the exact same position. Since
        2016 UV197 is no longer an recognized designation, 2014 EX61 was assumed to be the actual
        object.

        Lo 2020                        2016 UV197 may have been the designation at the time. Using
                                       the MPC MP Checker, the astrometric position from Lo et al.
                                       (2020), 2014 EX61 has the exact same position. Since 2016
                                       UV197 is no longer an recognized designation, 2014 EX61 was
                                       assumed to be the actual object.


      0 2014 ET121                    
        Lo 2020                        The designation at the time was likely 2016 UG159, which
                                       appears and shows the same position as 2014 ET121 in the MPC
                                       MPChecker. However, 2016 UG159 is no longer an assigned
                                       designation and so 2014 ET121 was used for this object.


      0 2014 GN1                      
        Hicks 2014d                    V-R = 0.40 assumed to give H = 24.1


      0 2014 JO25                     
        Aznar 2019b                    The primary record for Aznar 2019b gives the best-fit for the
                                       entire data set. The subsequent entires are based on subsets
                                       obtained by different observers throughout the runs of 2017
                                       April 20 to May 17.

        Venkataramani 2019             The actual phange angle ranged from 61 to 50 degrees over the
                                       course of the observations. During that time, the B-V color
                                       index increased (bluer) from 0.61 to 0.98 while the V-R index
                                       remained nearly constant.


      0 2014 MK6                      
        Navarro-Meza 2019              This note applies to all Navarro-Meza 2019 color index
                                       entries. The paper gave r-i colors after substracting solar
                                       color but that value was not given. A value of r-i(sun) =
                                       0.11(*) mag was added to the values in the paper for the
                                       listings in the color index tabel.
                                       http://classic.sdss.org/dr5/algorithms/sdssUBVRITransform.htm
                                       l


      0 2014 SC324                    
        Warner 2015h                   P2 in NPAR table is not unique. Low amplitude tumbler:
                                       A2/A1_secondharmonic ~ 0.21.


      0 2014 VR4                      
        Pravec 2019b                   Paired with (46829) McMahon.


      0 2014 WK368                    
        The albedo error given for Masiero 2018a is the maximum possible value when converting
        albedo values from log space to value space. The phase angle in the details record is from
        the file; the actual date of observation was not given.

        Masiero 2018a                  The albedo error given for Masiero 2018a is the maximum
                                       possible value when converting albedo values from log space
                                       to value space. The phase angle in the details record is from
                                       the file; the actual date of observation was not given.


      0 2015 AH1                      
        Pravec 2019b                   Paired with (16126) 1999 XQ86.


      0 2015 OH                       
        Warner 2016c                   Ambiguous: P_alt: 2.630 cannot be formally excluded but is
                                       not likely.


      0 2015 OS35                     
        Ieva 2018                      Computed phase angle significantly different from that in
                                       paper. Possible wrong date or object.


      0 2015 RF36                     
        Taylor 2015b                   Period estimated from spread of CW radar data


      0 2016 AZ8                      
        Virkki 2019                    The periods are based on upper limits and accounting for the
                                       mutual orbit plane being inclined several tens of degrees
                                       from the line of sight.

        Warner 2019m                   The orbital period is based on the lightcurve having the
                                       expected mutual events. The primary period seems much too
                                       long compared to initial radar observations.


      0 2016 BU13                     
        Warner 2016m                   Suspected P3 = 16.46 ± 0.02, A3 = 0.04 ± 0.01


      0 2016 CA138                    
        Borisov 2023                   Sidereal periods (h):  Pole 1: 5.3137 Pole 2: 5.3141 Pole 3:
                                       5.3139 Pole 3 mirror: 5.3139


      0 2016 EV27                     
        Warner 2016j                   Second period may be artificat of Fourier analysis. However,
                                       the two periods do not have a simple integral multiple ratio.
                                       


      0 2016 UW187                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2016 UZ215                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2016 UC230                    
        The object was determined using astrometric positions from Lo et al. (2020). However,
        because of significant deviation from given position and that found in the MPC MPChecker,
        this may not be the actual object that was observed.

        Lo 2020                        The object was determined using astrometric positions from Lo
                                       et al. (2020). However, because of significant deviation from
                                       given position and that found in the MPC MPChecker, this may
                                       not be the actual object that was observed.


      0 2017 BW                       
        Pravec 2017web                 Second period is no unique. First period could be rotation or
                                       precession.


      0 2017 NH                       
        Warner 2018a                   Second NPA period is one of many possibilities.


      0 2017 SL16                     
        Borisov 2023                   Sideral period for each pole: (190.4,34.3,0.3188)
                                       (183.7,-75.8,0.3190) (233.6,53.6,0.3192) (97.2,-41.2,0.3191)
                                       


      0 2017 YH                       
        Rondon 2022                    The observation date is the first in the set of observations,
                                       which spanned more than a year. The phase angle range was
                                       87.1-90.3 deg.


      0 2017 YE5                      
        JPL 2018                       Each body about 900 m, widely separated (~2500 m).


      0 2018 AJ                       
        Warner 2018k                   Second period may be actual second period or linear
                                       combination of the two frequencies of NPA rotation with the
                                       main frequency.


      0 2018 CB                       
        Birtwhistle 2021a              The phase angle for the breakout entries was forced to the
                                       mid-phase angle of the observations. The phase angle bisector
                                       values are for 00:00h UT on 2018 Feb 9.


      0 2018 JE1                      
        Warner 2018m                   Secondary period is likely wrong, even spurious. It was
                                       needed to overcome an excessively large nightly zero point
                                       shift of 0.8 mag.


      0 2018 KE3                      
        Warner 2019b                   Possible very wide binary, in which case the primary period
                                       is the longer of the two. The shorter period is rated U=3;
                                       the secondary period is U=2.


      0 2018 LK                       
        Warner 2018m                   Period is for combined data set from 2018 June 12-13.
                                       Individual results are reported seperatedly.


      0 2018 TF3                      
        Pravec 2018b                   The secondary period/amplitude given in the LC_BINARY table
                                       are for the synchronous satellite.

        Warner 2019f                   Orbital period derived from half-period analysis that allowed
                                       full coverage of the P_orb lightcurve.


      0 2018 UQ1                      
        Lopez-Oquendo 2019a            Longer solution of 7.1 h is likely a double-period fit by
                                       exclusion.


      0 2018 UD3                      
        Beniyama 2022                  Given the amplitude and assuming the original period is
                                       correct, the true period may be ~0.0165112 h.


      0 2018 XV5                      
        Pravec 2022web                 Amplitude for P2 (A2) not given so listed as the same as P1.

        Warner 2022i                   Periods 2 and 3 are artifacts of additive period analysis,
                                       which does not properly handle tumbling asteroids.


      0 2019 FP2                      
        Warner 2019p                   Extrmely noisy data with no discernible trends.


      0 2019 KZ3                      
        Warner 2019p                   A nearly as-good single period solution could also be found.
                                       The RMS scatter was higher by about 0.04 mag.


      0 2019 SH6                      
        Warner 2020c                   Two periods given were derived from subtracting an 8.22 h,
                                       0.19 mag lightcurve. This may be a 'beat frquency' period.


      0 2019 UC                       
        A super-short period (Pravec et al., 2019) is a possibility.


      0 2020 AZ2                      
        Pravec 2020b                   Satellite A = 0.07 mag, a/b = 1.23.


      0 2020 BX12                     
        Virkki 2020                    Diameter of 180 m is for projected-area-equivalent.
                                       Primary/Second sizes: 165 m and 70 m. An orbital period of
                                       15-16 not ruled out.


      0 2020 HS7                      
        Beniyama 2022                  Two observations on same date: midtimes: 14:36:31 amd
                                       16:24:21.


      0 2020 KK7                      
        Birtwhistle 2021a              H-G were determined using the lightcurve peak instead of
                                       average.


      0 2020 ST1                      
        Warner 2021d                   Pravec found the strongest solutions to be 1.879, 2.879, and
                                       5.407 h. Two are real, the third is related to the other two.
                                       Note that 1/2.879 = 1/1.879 - 1/5.407.


      0 2020 TP1                      
        Birtwhistle 2021e              The stated period and secondary in the NPAR table are not
                                       secure but simply two dominant periods found using software
                                       that properly handles tumbling asteroids.


      0 2021 DW1                      
        Kwiatkowski 2021               SG-SI: 0.79 Â± 0.01. The phase angle values are for 0h UT on
                                       the given date. They can be significantly different from the
                                       value at the actual time of observations.


      0 2021 DX1                      
        Warner 2021h                   The second period in the NPA table is one of several
                                       possibilities.


      0 2021 KN2                      
        Birtwhistle 2021c              P3: 0.012516(2) h, A3: 0.27.  1/P1 = 2/P3 - 2/P2


      0 2022 DA                       
        Period/amplitude could not be determined.

        Birtwhistle 2022b              Period/amplitude could not be determined.


      0 2022 LV                       
        Pravec 2022web                 Amplitude for P2 (A2) assumed to be the same as A1.


      0 2022 NE                       
        Birtwhistle 2023a              P3 = 0.01217 Â± 0.00001 h; A3 = 0.4 Â± 0.4 mag.


      0 2022 QT7                      
        Birtwhistle 2023a              P3 = 0.0147778 Â± 0.0000015 h; A3 = 0.7 Â± 0.5 mag.


      0 2023 HK                       
        Birtwhistle 2023d              The phase angle ranged from 50.5 to 72.3 over the span of the
                                       observations. The full range of the tumbling amplitude is
                                       ~1.5 mag.


      0 2023 HU4                      
        Birtwhistle 2023d              The second period is ambiguous. An alternate solution is P2 =
                                       0.1714 (0.0003) h, A = 0.4 (0.2) mag. The phase angle ranged
                                       from 15.0-11.8 deg over the span of the observations. The
                                       full range of the tumbling amplitude is ~1.3 mag.


      0 2023 HO18                     
        Birtwhistle 2023d              The phase angle ranged from 41.8 to 17.1 deg over the span of
                                       the observations. Using default G = 0.15 led to an offset of
                                       0.44 mag between two night and significant deviation from the
                                       predicted magnitudes using G = 0.15..


      0 2023 KZ1                      
        Birtwhistle 2023d              Indications of a long secondary period. Based on the raw
                                       plot, a solution might be P2 ~ 0.24 h for a bimodal curve
                                       [LCDB authors].


      0 C/2003 WT42                   
        Determined to be a comet after discovery and given asteroid designation. Current MPC
        designation is C/2003 WT42.


      0 Derm0a                        
        Dermawan 2002b, Doctoral Thesis This paper included approximately 50 objects, named in this
        list as DermXx, with X being a number and x a letter. The paper used the following values,
        which were adopted in lieu of the defaults used in this publication that are based on the
        semi-major axis:  SMA: 2.3 < a < 2.8, Type = C, V-R = 0.53±0.04, Pv = 0.21±0.05;   SMA: 2.8
        < a < 3.3, Type = C, V-R = 0.37±0.03, Pv = 0.06±0.02.  The listed diameters are those listed
        by Dermawan as computed from these assumed values and his measured value of Hv.


      0 Derm1c                        
        Dermawan 2011                  Only 22 data points.


      0 Derm2b                        
        Dermawan 2011                  D flag applies to amplitude only.


      0 Derm2h                        
        Dermawan 2011                  D flag applies to amplitude only.


      0 Derm2K                        
        Dermawan 2011                  Only 18 data points.


      0 Derm2O                        
        Dermawan 2011                  Only 9 data points.


      0 Derm3b                        
        Dermawan 2011                  Any number of period solutions are possible.


      0 Derm4m                        
        Dermawan 2011                  Dermawan paper gave amplitude as A = 0.35. It should have
                                       been 0.035. The value was rounded up to 0.04 mag for entry.


      0 Derm6e                        
        Dermawan 2011                  R = 24.


      0 Derm6j                        
        Dermawan 2011                  R = 24.


      0 FOSL01010327                  
        Chang 2022b                    This applies to all Chang 2022b; Ap. J. Suppl. Ser. 259,
                                       id.7. The filter band was r2 for all observations other than
                                       Apr 10, 2019, which used the SG filter. 'r2' is not
                                       recognized in the LCDB, so SR (Sloan r') is given. The
                                       reported diameters do not always agree with the standard
                                       formula using H and albedo to find a diameter. The summary
                                       line uses the value of the standard formula.


      0 FSAP04010083                  
        This note applies to all Chang 2021 (PSJ 2) entries. The observations were made in g and r2
        bands. The photometric bands (for H) were assigned as SG and SR, respectively. The H_SR
        values were transformed to approximate V by using the LCDB V = SR+ 0.22. While not exact,
        this makes the values more compatible to H_V when plotting frequency-diameters. For diameter
        calculations, an albedo of 0.05 and G = 0.15 Ã‚Â± 0.2 was assumed for both bands. Only some
        of the 53 objects could be tied to an object in the MPC database. For those without ID, and
        where possible, the phase and phase angle bisector values were assumed to be the same as for
        an identified object in the same observing block. The entries are flagged as being from a
        Sparse Wide-field Survey (SWF).


      0 FSAP04010100                  
        This applies only to Chang et al. (2021) Plan. Sci. J. 2, id.191. Many of the objects were
        not tied to known Hildas. As a result, the orbital parameters were not available and,
        therefore, the phase angle bisector and phase angles could not be calculated. Generally, the
        phase angle for any Hilda group member is <20 degrees.

        Chang 2022b                    This applies to all Chang et al. (2021) Plan. Sci. J. 2,
                                       id.191. Many of the objects were not tied to known Hildas. As
                                       a result, the orbital parameters were not available and,
                                       therefore, the phase angle bisector and phase angles could
                                       not be calculated. Generally, the phase angle for any Hilda
                                       group member is <20 degrees.


      0 Himalia                       
        Mainzer 2011                   The diameters and H values were taken from other sources and
                                       then used to calibrate expected errors in diameters and
                                       albedo derived from WISE data.


      0 P/2006 HR30                   
        Determined to be a comet after initial discovery and asteroid designation (2006 HR30).
        Current MPC designation is P/2006 HR30.


      0 P0007F                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


      0 P00095                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


      0 P000DV                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000K7                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000ZE                        
        Polishook 2012b                Object could not be tied to one in MPCORB file.


      0 P000ZL                        
        Polishook 2012b                Object could not be tied to one in the MPCORB file.


