Small Bodies Node

Asteroid 1379 Lomonosowa (top)

2MASS Asteroid and Comet Survey V2.0 (1 data product)

J MAGNITUDE 2MASS * J band selected magnitude in the 2MASS survey, or if the source is not detected in the J-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the first character of the rd_flg value. (MAGNITUDE)	J MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the J-band magnitude in the 2MASS survey. If rd_flg[1]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[1]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If J_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[1]=0 or 6) or if the source is not measurable (rd_flg[1]=9). (MAGNITUDE)	H MAGNITUDE 2MASS * H band selected magnitude in the 2MASS survey, or if the source is not detected in the H-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the second character of the rd_flg value. (MAGNITUDE)	H MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the H-band magnitude in the 2MASS survey. If rd_flg[2]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[2]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If H_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[2]=0 or 6) or if the source is not measurable (rd_flg[2]=9). (MAGNITUDE)	KS MAGNITUDE 2MASS * Ks band selected magnitude in the 2MASS survey, or if the source is not detected in the Ks-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the third character of the rd_flg value. (MAGNITUDE)	KS MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the Ks-band magnitude in the 2MASS survey. If rd_flg[3]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[3]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If KS_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[3]=0 or 6) or if the source is not measurable (rd_flg[3]=9). (MAGNITUDE)
12.851	0.023	12.484	0.026	12.400	0.032

Asteroid 1379 Lomonosowa (top)

Asteroid Absolute Magnitudes V12.0 (1 data product)

ABSOLUTE VISUAL MAGNITUDE * IAU-adopted absolute V magnitude (H) (MAGNITUDE)	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
11.05	0.15	a	MPC 17262

Asteroid 1379 Lomonosowa (top)

Asteroid Dynamical Families V4.1 (2 data products)

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.

WILLIAMS FAMILY * Family identification according to the Williams analysis	KOZAI FAMILY * Family identification according to the Kozai analysis	CARUSI FAMILY * Family identification according to the Carusi and Massaro analysis	LINDBLAD SOUTHWORTH FAMILY * Family identification according to the Lindblad and Southworth analysis	VAN HOUTEN FAMILY * Family identification according to the van Houten analysis	ARNOLD FAMILY * Family identification according to the Arnold analysis	BROUWER FAMILY * Family identification according to the Brouwer analysis	HIRAYAMA FAMILY * Family identification according to the Hirayama analysis	ZAPPALA FAMILY * Family identification according to the Zappala analysis
	17				4	4

Asteroid 1379 Lomonosowa (top)

Asteroid Lightcurve Derived Data V16.0 (2 data products)

LC PERIOD FLAG * Flag referring to the sidereal period given in the asteroid lightcurve parameters file, taking the following values: > - less than	LC PERIOD * 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. (HOUR)	LC PERIOD ERR * Error in the rotational period given in the asteroid lightcurve parameters file. (HOUR)	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. - greater than	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. (MAGNITUDE)	LC AMPLITUDE ERR * Error in the lightcurve amplitudes given in the asteroid lightcurve parameters file. (MAGNITUDE)	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 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.
						.	I	Masiero 2012
	24.488	0.001		0.63	0.02	3		Brinsfield 2008e
						.	I	AKARI
						.	I	WISE
	24.4825	0.0272		0.45		2		Waszczak 2016
						.	N	Veres 2015
S	24.4846	0.0001				2	N	Durech 2016
	24.71		>	0.51		2		Binzel 1987b
S	24.4845	0.0005				.	N	Hanus 2011

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.	LC SPINAXIS QUALITY CODE * The Q value gives our assessment of the quality of the pole solution. 0 Either wrong or very uncertain determination 1 Possible but not certain pole determination. This will most often appear when a limited number of data sets is used, especially if methods other than lightcurve inversion are involved. 2 Good determination, based on large dataset. The solution consists of one or two solutions (and possibly their 180 degree mirrors). If two solutions, they may differ in both longitude and latitude but not by the simple 180 degree mirror. 3 Very good determination, based on large dataset, an ambiguity of about 180 degrees in pole longitude might appear. 4 Excellent determination, pole position confirmed by methods based on independent datasets (for example, lightcurves and radar data, lightcurves and spacecraft fly-by). P A prograde rotation has been determined but no specific pole position has been determined. This will be followed by a 0 or 1, indicating the quality of the determination. R A retrograde rotation has been determined by no specific pole position has been determined. This will be followed by a 0 or 1, indicating the quality of the determination. In some cases, the numerical quality code is 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. If the Q value is blank, the given pole solution has not yet been reviewed under the new rating system.	LC PERIOD * 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. (HOUR)	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. (MAGNITUDE)	LC SPINAXIS ECLIPTIC LONGITUDE 1 * Ecliptic longitude of the first solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LATITUDE 1 * Ecliptic latitude of the first solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LONGITUDE 2 * Ecliptic longitude of the second solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LATITUDE 2 * Ecliptic latitude of the second solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS SIDEREAL PERIOD * Sidereal period of the spinaxis solution in the spinaxis file of the asteroid derived lightcurve data set. (HOUR)	LC SPINAXIS SHAPE FLAG * Flag for shape model in the spinaxis file of the asteroid derived lightcurve data set: Y = shape model exists
summary	9+	24.488	0.63
Hanus 2011	R				-62.0			24.4845
Durech 2016	9+			72.0	-84.0	265.0	-46.0	24.4846	Y

Asteroid 1379 Lomonosowa (top)

Asteroid Names and Discovery V12.0 (1 data product)

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
1936-03-19	Simeis	Neujmin, G.

Asteroid 1379 Lomonosowa (top)

Asteroid Photometric Catalog V1.1 (4 data products)

001379_19840307014927_V_TAB

time: 1984-03-07T01:49:27 file: indiv/ast001379/19840307014927_v.tab dataset: Asteroid Photometric Catalog V1.1

The Asteroid Photometric Catalog is intended to be a compilation of all published photometric data on lightcurves of asteroids. This dataset includes the third update to the APC, and is therefore complete through 1992. This file contains a single asteroid lightcurve.

001379_19840307023412_V_TAB

time: 1984-03-07T02:34:12 file: indiv/ast001379/19840307023412_v.tab dataset: Asteroid Photometric Catalog V1.1

The Asteroid Photometric Catalog is intended to be a compilation of all published photometric data on lightcurves of asteroids. This dataset includes the third update to the APC, and is therefore complete through 1992. This file contains a single asteroid lightcurve.

001379_19840307052356_V_TAB

time: 1984-03-07T05:23:56 file: indiv/ast001379/19840307052356_v.tab dataset: Asteroid Photometric Catalog V1.1

The Asteroid Photometric Catalog is intended to be a compilation of all published photometric data on lightcurves of asteroids. This dataset includes the third update to the APC, and is therefore complete through 1992. This file contains a single asteroid lightcurve.

001379_19840307084658_V_TAB

time: 1984-03-07T08:46:58 file: indiv/ast001379/19840307084658_v.tab dataset: Asteroid Photometric Catalog V1.1

The Asteroid Photometric Catalog is intended to be a compilation of all published photometric data on lightcurves of asteroids. This dataset includes the third update to the APC, and is therefore complete through 1992. This file contains a single asteroid lightcurve.

Asteroid 1379 Lomonosowa (top)

Asteroid Taxonomy V6.0 (1 data product)

THOLEN CLASS * Taxonomic classification according to the method of Tholen (1984, 1989). An entry with the value of '***' indicates an object with unusual colors not classifiable into any of the defined classes.	BARUCCI CLASS * Taxonomic classification according to the method of Barucci et al. (1987).	TEDESCO CLASS * Taxonomic classification according to the method of Tedesco et al. (1989).	HOWELL CLASS * Taxonomic classification according to the method of Howell (1994).	SMASS CLASS * Taxonomic classification based on the spectra of the SMASS survey (Xu et al. 1995).	BUS CLASS * Taxonomic classification based on the spectra of the SMASSII survey (Bus and Binzel 2002). An entry with a value of '***' indicates the object has an unusual spectrum not classifiable into any of the defined classes.	S3OS2 CLASS TH * Taxonomic classification based on the spectra of the S3OS2 survey and using the method of Tholen (1984). For details of how the method was applied, see [LAZZAROETAL2004] (Icarus 172, 179-220.)	S3OS2 CLASS BB * Taxonomic classification based on the spectra of the S3OS2 survey and using the method of Bus and Binzel (2002). For details of how the method was applied, see [LAZZAROETAL2004] (Icarus 172, 179-220.)	BUS DEMEO CLASS * Taxonomic classification from DeMeo et al. (2009). Note that a 'w' following the taxonomic class indicates a slope greater than 0.25, and a ':' indicates a questionable classification because of low quality/questionable data.
				S

Asteroid 1379 Lomonosowa (top)

Fieber-Beyer IRTF Mainbelt Asteroid Spectra V2.0 (3 data products)

SPECTRUM 1379 LOMONOSOWA

time: 2008-05-20T05:53:05Z file: fieberbeyer2010/1379.tab dataset: Fieber-Beyer IRTF Mainbelt Asteroid Spectra V2.0

The data set contains observations obtained with the NASA IRTF SpeX instrument covering the 0.7-2.5 micron near-infrared portion of the spectrum. The data set archives reduced, calibrated spectra which were obtained and used in Sherry Fieber-Beyer's Ph.D. dissertation at the University of North Dakota. The research focused on asteroids in a zone centered on the 3:1 resonance. These spectra were used to mineralogically characterize asteroids in this zone in an attempt to identify their meteorite analogs.

Asteroid 1379 Lomonosowa (top)

Fieber-Beyer IRTF Mainbelt Asteroid Spectra V3.0 (1 data product)

SPECTRUM 1379 LOMONOSOWA

time: 2008-05-20T05:53:05 file: fieberbeyer2010/1379.tab dataset: Fieber-Beyer IRTF Mainbelt Asteroid Spectra V3.0

The data set contains observations obtained with the NASA IRTF SpeX instrument covering the 0.7-2.5 micron near-infrared portion of the spectrum. The data set archives reduced, calibrated spectra which were obtained and used in Sherry Fieber-Beyer's Ph.D. dissertation at the University of North Dakota. The research focused on asteroids in a zone centered on the 3:1 resonance. These spectra were used to mineralogically characterize asteroids in this zone in an attempt to identify their meteorite analogs.

Asteroid 1379 Lomonosowa (top)