Download LCDB README.TXT for explanations of field names and data

LCDB References table with BibCode links to ADS

To shorten some field names, 'SOURCE' is reduced to 'S' and 'FLAG' is reduced to 'F'.
For example, 'HSOURCE' is 'HS'.

BibCode links open a new window


2181442002 RL662002 RL66MCASC 2.97M15.0 M0.15A 0.20 587.  0.250.323-T0 ? 0 


ReferenceBibCodeWorked asDateObs    PABLPABBPhaseFamilyClassDiamMethDiamFDiamDiamErrHSHHErrHBandGSGGErrAlbSAlbFAlbedoAlbErrPFPeriodPerErrPerDescAmpFAmpMinAmpMaxAmpErrUNotesPoleBINSurveyIsPrivateNotesEx
Warner 2010e2010MPBu...37...57W2002 RL662010-02-01100.835.735.0                  590.5.   0.320.022+T0   0See footnotes
Warner 2010m2010MPBu...37..109W2002 RL662009-12-3188.436.431.2                  587.10.   0.250.023-T0 ? 0See footnotes
Ali-Lagoa 20172017A&A...603A..55A2002 RL662010-04-10135.322.036.1    2.460.25A15.00  A0.15   0.2910.058         I   0 
Popescu 2018b2018A&A...617A..12P2002 RL66    MCV                        I   0 

Details Notes
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.


Warner 2010m2010MPBu...37..109WA587.         

Tumbling (NPAR)

Warner 2010e2010MPBu...37...57W0    
Warner 2010m2010MPBu...37..109W0