ABSOLUTE VISUAL MAGNITUDE
* IAU-adopted absolute V magnitude (H)
|SLOPE PARAMETER * IAU-adopted slope parameter (G)||SLOPE PARAMETER ORIGIN FLAG * Those slope parameters that were determined by fitting the IAU-adopted phase function to data are given an origin code letter of 'f' (for 'fitted'); all others are given a code letter of 'a' (for 'assumed').||MPC REFERENCE * Minor Planet Circular (MPC) or Minor Planet Orbit Supplement (MPO) reference|
|ZAPPALA FAMILY NAME * Familiy name in the family analysis of Zappala et al. (1995)||ZAPPALA CLUMP FLAG * Indicates whether the Zappala family designation is a clump or a family, as defined in Zappala et al. (1995). F = family, C = clump.||ZAPPALA FAMILY CONFIDENCE LEVEL * Confidence level of Zappala family membership, defined as quality code (QC) in Zappala et al. 1995.|
|LC PERIOD FLAG * Flag referring to the sidereal period given in the asteroid lightcurve parameters file, taking the following values: > - less than < - greater than D - no numeric value (see P_NOTE for details) S - sidereal period (default is synodic period) U - period uncertain This is not the same as ambiguous where one or more additional periods are reported.||LC PERIOD NOTE * Note with further information about the period given in the asteroid lightcurve parameters file.||
* Rotation period of the asteroid about its axis, in hours, in the asteroid lightcurve parameters file. The period given is synodic unless the S flag (sidereal) is set in P_FLAG.
LC PERIOD ERR
* Error in the rotational period given in the asteroid lightcurve parameters file.
|LC AMPLITUDE FLAG * A flag pertaining to the amplitude of the lightcurve in the asteroid lightcurve parameters file, given in AMP_MIN and AMP_MAX. < - less than > - greater than||
LC AMPLITUDE MINIMUM
* Lightcurve amplitude minimum, in the asteroid lightcurve parameters file. In the cases where a range of amplitude is given, this is the lower limit of the range. For individual observations for which a single value of the amplitude is given, this field contains a null value.
LC AMPLITUDE MAXIMUM
* Lightcurve amplitude maximum in the asteroid lightcurve parameters file. In cases where a range of amplitudes is given, this field is the upper limit of the range. In cases where a single value is given for the amplitude, this field is that value and a null value is given for AMP_MIN. Both AMP_MIN and AMP_MAX contain a null value if the publication did not include an amplitude.
LC AMPLITUDE ERR
* Error in the lightcurve amplitudes given in the asteroid lightcurve parameters file.
|LC QUALITY CODE * This code describes the reliability of the lightcurve results in the asteroid lightcurve parameters file, and takes the following values: 0 - Result later proven incorrect. This appears only on records of individual observations. 1 - Result based on fragmentary lightcurve(s), may be completely wrong. 2 - Result based on less than full coverage, so that the period may be wrong by 30 percent or so. Also, a quality of 2 is used to note results where an ambiguity exists as to the number of extrema per cycle or the number of elapsed cycles between lightcurves. Hence the result may be wrong by an integer ratio. 3 - Denotes a secure result with no ambiguity and full lightcurve coverage. 4 - In addition to full coverage, denotes that a pole position is reported. In some cases, the numerical quality code may be followed by a plus or minus sign, indicating that the reliability is judged somewhat better (+) or worse (-) than implied by an un-signed number alone. This refinement in scale has been only recently added, and not yet retroactively, so most entries don't have signs, even in some cases where they would be appropriate.||LC NOTES * Notes pertaining to the lightcurve reported in the asteroid lightcurve parameters file. These are one-letter flags, one or more of which may appear in the column. ? - Usually tied with 'T' to indicate uncertainty. 1 - Monomodal curve (one min/max per rotation) 3 - Trimodal curve (three min/max per rotation) 4 - Quadrimodal curve (four min/max per rotation) A - Ambiguous period D - Period determined by us that differs from that given in the original publication E - Occultation observation H - Space telescope observations I - IR/Thermal observations M - Polarimetric observation N - No lightcurve published O - Adaptive optics observation P - Photographic photometry R - Radar observation T - Tumbling (Non-principal axis rotation - see lc_npa.tab for details) V - Visual photometry Additional flags associated with the T flag are as follows: None after the T - The asteroid is definitely tumbling ? : Possible tumbler 0 : The tumbling damping timescale is long enough that tumbling might be expected, but observations are not sufficient to substantiate either tumbling or not tumbling. - : The tumbling damping timescale is long enough that tumbling might be expected, but observations indicate the object is NOT tumbling. + : The tumbling damping timescale is short enough that tumbling would not seem likely, however, observations indicate that it may be tumbling or actually is tumbling.||LC BINARY FLAG * Note regarding binarity in the asteroid lightcurve parameters file: ? - Possible, usually due to lacking mutual eclipse/occultation events B - Binary system M - Multiple system, more than two||LC REFERENCE ID * A short version of the reference citation for the published paper in which the values in this entry (in the asteroid lightcurve parameters file) were reported. The full citations may be found in the file lc_references.tab.|
|DISCOVERY DATE * Date of discovery of an object||DISCOVERY LOCATION * Location where the discovery observation of an object was made||DISCOVERER NAMES * The name(s) of the discoverer(s) of an object|
|1980-06-11||Flagstaff (AM)||Bowell, E.|
|SIMPS MEAN ALBEDO * Mean derived geometric albedo on the H,G system from the Supplemental IRAS Minor Planet Survey (SIMPS).||SIMPS MEAN ALBEDO UNC * 1-sigma uncertainty in the mean derived geometric albedo from the Supplemental IRAS Minor Planet Survey (SIMPS), due solely to the precision of the IRAS flux data.||
SIMPS MEAN DIAMETER
* Mean diameter from the Supplemental IRAS Minor Planet Survey (SIMPS), computed from H and SIMPS_MEAN_ALBEDO
|SIMPS MEAN DIAMETER UNC * 1-sigma uncertainty in the mean diameter from the Supplemental IRAS Minor Planet Survey (SIMPS), due solely to the precision of the IRAS flux data.||SIMPS PLC * Probability of lightcurve variation, estimated in the Supplemental IRAS Minor Planet Survey (SIMPS). This quantity is used as a measure of the probability that a lightcurve effect is present in the data. Values are constrained to be between 0.10 and 1.00. Less than significant variation is assigned a value of 0.10.|
|MK RESONANCE FLAG * Resonance flag as defined in Milani and Knesevic 1994, Icarus 107, 219.||MK MEAN ELEMENTS QUALITY CODE * Mean elements quality code as defined in Milani and Knesevic 1994, Icarus 107, 219.||MK OSCULATING ELEMENTS QUALITY CODE * Osculating elements quality code as defined in Milani and Knesevic 1994, Icarus 107, 219.||MOTHEFAM FAMILY MEMBERSHIP * The family membership as defined in the Mothe-Diniz et al. asteroid family data set.|
* NEOWISE best-fit effective spherical diameter, or assumed value if not fitted.
NEOWISE DIAMETER UNCERTAINTY
* NEOWISE unceratinty in the best-fit effective spherical diameter, or assumed value if not fitted.
|NEOWISE V ALBEDO * NEOWISE best-fit visible geometric albedo, or assumed value if not fitted.||NEOWISE V ALBEDO UNCERTAINTY * NEOWISE uncertainty of the best-fit visible geometric albedo, or assumed value if not fitted.||NEOWISE THERMAL BEAMING PARAMETER * NEOWISE best-fit NEATM thermal beaming parameter, or assumed value if not fitted.||NEOWISE THERMAL BEAMING PARAMETER UNCERTAINTY * NEOWISE uncertainty of the best-fit NEATM thermal beaming parameter, or assumed value if not fitted.||NEOWISE REFERENCE CODE * NEOWISE reference code to the original publication of fitted parameters. See the refrence.tab in the dataset for the full reference|
|NESVORNY SYNTHETIC FAMILY NUMBER * Family number assigned for the purpose of the Nesvorny family analysis based on synthetic proper elements. Family numbers in the 400's refer to inner belt families, in the 500's to central belt families, and in the 600's to outer belt families. High inclination families from synthetic proper elements have family numbers in the 700's for the inner belt, the 800's for the central belt, and the 900's for the outer belt.||NESVORNY SYNTHETIC FAMILY NAME * The name of the asteroid family in the Nesvorny family analysis based on synthetic proper elements. The family name is based on the name or provisional designation of the largest member of the family.|