Small Bodies Node

Asteroid 20 Massalia (top)

24-Color Asteroid Survey (1 data product)

20MASSALIA

time: N/A file: data2/20massalia.tab dataset: 24-Color Asteroid Survey

This file contains the spectrum of the asteroid specified in TARGET NAME, as part of the 24-color Asteroid Survey.

Asteroid 20 Massalia (top)

52-Color Asteroid Survey (1 data product)

20MASSALIA

time: N/A file: data1/20massalia.tab dataset: 52-Color Asteroid Survey

This table contains a 52-color IR spectrum of the asteroid specified in TARGET_NAME.

Asteroid 20 Massalia (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
6.50	0.25	f	MPC 17257

Asteroid 20 Massalia (top)

Asteroid Albedos (1 data product)

MIMPS ALBEDO * Mean geometric visual albedo on the H,G magnitude system, from the MSX Infrared Minor Planet Survey (MIMPS).	MIMPS ALBEDO UNC * 1-sigma uncertainty in the mean geometric visual albedo from the MSX Infrared Minor Planet Survey (MIMPS).
0.2096	0.030

Asteroid 20 Massalia (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.
Massalia	F	3

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
162	15							Massalia

Asteroid 20 Massalia (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 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. (MAGNITUDE)	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.
	8.09867	0.00008		0.22	0.01	3		Higgins 2012web
						.	I	Masiero 2012
						.	I	AKARI
S	8.09759	0.00005				.	N	Hanus 2016
						.		Krugly 1992
						.		Lagerkvist 1989
S	8.098					.		Magnusson 1986
				0.21		.		McCheyne 1985
	8.0994			0.15		.		Belskaya 2003
						.	N	Lagerkvist 1988
				0.20		.		Lupishko 1982b
						.		Bianchi 1921
	8.098		0.17	0.23		3		Gehrels 1956
				0.24		.		Gehrels 1962
				0.18		.		Vesely 1985
						.	I	SIMPS
						.		Lim 2005
				0.20		.		Zhou 1982
	8.093			0.26		.		Hainaut-Rouelle 1995
	8.098		0.24	0.27		3		Chang 1962
S	8.09757					.		Szabo 1999
S	8.097714					.		Kaasalainen 2002a
S	8.09759					.		Dotto 1995
				0.18		2		Barucci 1985

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 ECLIPTIC LONGITUDE 3 * Ecliptic longitude of the third solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LATITUDE 3 * Ecliptic latitude of the third solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LONGITUDE 4 * Ecliptic longitude of the fourth solution in the spinaxis file of the asteroid derived lightcurve data set (DEGREE)	LC SPINAXIS ECLIPTIC LATITUDE 4 * Ecliptic latitude of the fourth 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+	8.098	0.27
Chang 1962	9+			10.0	78.0	190.0	-78.0
Barucci 1985	9+			30.0	49.0	207.0	51.0	27.0	-51.0	210.0	-49.0		Y
McCheyne 1985	9+			30.0	54.0	205.0	79.0	25.0	-79.0	210.0	-54.0		Y
Magnusson 1986	9+			20.0	80.0	200.0	80.0					8.098
Krugly 1992	9+
Dotto 1995	9+			31.0	69.0	208.0	69.0					8.09759	Y
Szabo 1999	9+			27.0	38.0	207.0	38.0					8.09757	Y
Kaasalainen 2002a	2			179.0	39.0	0.0	40.0					8.09902	Y
Hanus 2016	9+			304.0	76.0							8.09759

Asteroid 20 Massalia (top)

Asteroid Masses V3.0 (1 data product)

ASTEROID MASS * The mass of an asteroid (KILOGRAM)	ASTEROID MASS UNC * Uncertainty in the asteroid mass (KILOGRAM)	ASTEROID DENSITY * The bulk density of an asteroid (GRAM_PER_CUBIC_CENTIMETER)	ASTEROID DENSITY UNC * Uncertainty in the asteroid density (GRAM_PER_CUBIC_CENTIMETER)	AXIS A * Long axis (not semi-axis) a of the ellipsoidal model approximating the size and shape of the body (KILOMETER)	AXIS B * Intermediate axis (not semi-axis) b of the ellipsoidal model approximating the size and shape of the body (KILOMETER)	AXIS C * Short axis (not semi-axis) c of the ellipsoidal model approximating the size and shape of the body (KILOMETER)	EQUIVALENT RADIUS UNC * Uncertainty in the size values AXIS_A, AXIS_B, and AXIS_C, stated as the uncertainty in the radius of the sphere with the equivalent volume. Note that AXIS_A, AXIS_B, and AXIS_C are semi-axes. (KILOMETER)	ASTMASS SIZE REFERENCE ID * A reference to the published source(s) of the size and shape parameters AXIS_A, AXIS_B, AXIS_C, and EQUIV_RADIUS_UNC in the asteroid masses data set. The full references are given in the file astmassrefs.tab.	ASTMASS REFERENCE ID * The reference for the published source of the asteroid mass and density information in this entry in the asteroid masses data set. The complete citations of the papers are given in the file astmassrefs.tab
4.77E+18	7.96E+17	2.98	0.76	160.000	145.000	132.000	4.650	Kaasalainen et al. 2002, Tedesco et al. 2002	Bange 1998
5.67E+18	8.15E+17	3.54	0.85	160.000	145.000	132.000	4.650	Kaasalainen et al. 2002, Tedesco et al. 2002	Baer et al. 2008
3.34E+18	6.96E+17	2.08	0.59	160.000	145.000	132.000	4.650	Kaasalainen et al. 2002, Tedesco et al. 2002	Baer et al. 2011

Asteroid 20 Massalia (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
1852-09-19	Naples	De Gasparis, A.

Asteroid 20 Massalia (top)

Asteroid Occultations V14.0 (1 data product)

OBSERVATION DATE * Date of observation	OCC MAJOR AXIS * Major axis of best-fit ellipse derived from stellar occultation observations (KILOMETER)	OCC MINOR AXIS * Minor axis of best-fit ellipse derived from stellar occultation observations (KILOMETER)	OCC MAJOR AXIS POSITION ANGLE * Position angle of major axis of best-fit ellipse derived from stellar occultation observations (DEGREE)	OCC FIT QUALITY CODE * Quality code for occultation fit: 0 - no fit, no position; 1 - no fit, but observations sufficiently reliable to derive an astrometric position of the asteroid relative to the star; 2 - poor fit; 3 - good fit; 4 - excellent fit	OCC MAJOR AXIS UNC * Standard deviation of major axis of best-fit ellipse derived from stellar occultation observations (KILOMETER)	OCC MINOR AXIS UNC * Standard deviation of minor axis of best-fit ellipse derived from stellar occultation observations (KILOMETER)	OCC MAJOR AXIS POSITION ANGLE UNC * Standard deviation of position angle of major axis of best-fit ellipse derived from stellar occultation observations (DEGREE)
2003-12-02	150.0	150.0	0.0	1
2009-04-22	157.0	157.0	0.0	2	7.6
2012-04-09	131.0	131.0	0.0	1
2012-10-09	128.0	77.0	93.7	2	5.4	8.0	2.5

Asteroid 20 Massalia (top)

Asteroid Photometric Catalog V1.1 (15 data products)

000020_19550327015951_V_TAB

time: 1955-03-27T01:59:51 file: indiv/ast000020/19550327015951_v.tab dataset: Asteroid Photometric Catalog V1.1