J/MNRAS/491/5966 V-types Main Set and HED meteorites catalogues (Mansour+, 2020)
Distribution and spectrophotometric classification of basaltic asteroids.
Mansour J.-A., Popescu M., De Leon J., Licandro J.
<Mon. Not. R. Astron. Soc., 491, 5966-5979 (2020)>
=2020MNRAS.491.5966M 2020MNRAS.491.5966M (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets ; Photometry, infrared ; Morphology
Keywords: techniques: photometric - techniques: spectroscopic - minor planets -
asteroids: general
Abstract:
We aim to determine the distribution of basaltic asteroids (classified
as V-types) based on the spectrophotometric data reported in the
MOVIS-C catalogue. A total of 782 asteroids were identified. The
observations with all four filters (Y, J, H, Ks), available for 297 of
these candidates, allow a reliable comparison with the laboratory data
of howardite, eucrite, and diogenite meteorites. We found that the
majority of the basaltic candidates (∼95 per cent) are located in the
inner main belt, while only 29 (∼4 per cent) and 8 (∼1 per cent) are
located in the middle (MMB) and outer main belt (OMB), respectively. A
fraction of ∼33 per cent from the V-type candidates is associated with
the Vesta family (with respect to AstDyS). We also identified four MMB
V-type candidates belonging to (15) Eunomia family, and another four
low inclination ones corresponding to (135) Hertha. We report
differences between the colour indices and albedo distributions of the
V-type candidates located in the inner main belt compared to those
from the MMB and OMB. These results support the hypothesis of a
different origin for the basaltic asteroids with a semimajor axis
beyond 2.5au. Furthermore, lithological differences are present
between the vestoids and the inner low inclination basaltic asteroids.
The data allow us to estimate the unbiased distribution of basaltic
asteroids across the main asteroid belt. We highlight that at least 80
per cent of the ejected basaltic material from (4) Vesta is missing or
is not yet detected because it is fragmented in sizes smaller than 1km.
Description:
The V-types Main Set and HED meteorites catalogues contain a number of
783 basaltic asteroid candidates selected from the MOVIS catalogue
(Popescu et al 2016, 2018) and a number of 245 Howardite, Eucrite and
Diogenite meteorites selected from the RELAB database (December 2014
catalogue version). The selection of the basaltic candidates is based
on restrictions on color indices. The proper orbital elements are
obtained from the AstDys (Milani et al., 2014, Icarus, 239, 46) and
Nesvorny et al. (2015, in Asteroids IV, Michel P., DeMeo F.E., Bottke
W.F., eds, Identification and Dynamical Properties of Asteroid
Families. Univ. Arizona Press, Tucson, AZ, p. 29) via the Planetary
Data System.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
vtypes.dat 349 782 V-type asteroids
hed-met.dat 292 244 HED meteorites
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See also:
J/ApJ/741/68 : Main Belt asteroids with WISE/NEOWISE. I. (Masiero+, 2011)
J/ApJ/792/30 : NEOWISE magnitudes for near-Earth objects (Mainzer+, 2014)
J/A+A/617/A12 : Taxonomic classification of asteroids (Popescu+, 2018)
Byte-by-byte Description of file: vtypes.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- Main Main Designation of the asteroids given by
the Minor Planet Center (MPC)
8-104 A97 --- Equiv Alternative designations that have been
given to the object
106-113 A8 --- Loc Location of the asteroid in the Main Belt
115-125 A11 --- Class Dynamical class based on Nesvorny et al.,
2008, Icarus, 193, 85
127-130 I4 --- Family Associated family of asteroids based on
AstDyS (Milani et al., 2014, Icarus, 239, 46),
the number corresponds to the most
representative asteroid in the family
132-140 A9 --- Type Associated lithology
142-149 E8.4 --- PHow ? Monte Carlo probability that an
asteroid is a howardite
151-158 E8.4 --- PEuc ? Monte Carlo probability that an
asteroid is a eucrite
160-167 E8.4 --- PDio ? Monte Carlo probability that an
asteroid is a diogenite
169-179 A11 km Diam Diameter
181-185 F5.3 km e_Diam ? Associated diameter error
187-191 F5.3 mag H Absolute magnitude
193-196 F4.1 --- AlbedoV Visible albedo recorded by the WISE survey (1)
198-206 F9.7 AU aprop ? Proper semi-major axis
208-216 F9.7 --- eprop ? Proper eccentricity
218-223 F6.3 deg iprop ? Proper inclination
225-233 F9.7 --- siniprop ? sinus of proper inclination
235-245 F11.9 mag Y-J Y-J Color index
247-257 F11.9 mag e_Y-J Error of the Y-J color index
259-271 F13.9 min Y-Jtmin Time interval between observation in Y band
and observation in J band
273-284 E12.9 mag J-K J-K Color index
286-296 F11.9 mag e_J-K Error of the J-K color index
298-309 F12.9 min J-Ktmin Time interval between observation in J band
and observation in K band
311-322 E12.9 mag H-K ? H-K color index
324-334 F11.9 mag e_H-K ? Error of the H-K color index
336-347 F12.9 min H-Ktmin ? Time interval between observation in H band
and observation in K band
349 A1 --- Taxon Taxonomical classification based on
Popescu et al.,
2018A&A...617A..12P 2018A&A...617A..12P, Cat. J/A+A/617/A12
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Note (1): Masiero et al., 2011ApJ...741...68M 2011ApJ...741...68M, Cat. J/ApJ/741/68,
Mainzer et al., 2014ApJ...792...30M 2014ApJ...792...30M, Cat. J/ApJ/792/30.
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Byte-by-byte Description of file: hed-met.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- SampleID Unique identification of each sample (1)
15- 25 A11 --- SpectrumID Associated spectrum ID
27- 38 F12.9 mag H-K Computed H-K color index, associated to the
spectrum of a meteorite
40- 51 F12.9 mag J-H Computed J-H color index, associated to the
spectrum of a meteorite
53- 87 A35 --- Origin The geographical site from which the sample
was obtained or where it was prepared
89-117 A29 --- Texture The physical form of the sample
(chip, particulate,thinsection, etc.)
119-121 I3 --- MinSize ?=- Minimum particle size;
zero if rock, slab, or thinsection
123-126 I4 --- MaxSize ?=- Maximum particle size;
zero if rock, slab, or thinsection
128-137 A10 --- Type General description of the type of meteorite
139-180 A42 --- Subtype Particular subtype of a meteorite group
182-292 A111 --- Com Additional comments
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Note (1): The format is XY-PII-NNN-ABC where
XY = Subcode, PII = PI initials, NNN = A sequence number,
ABC = Optional characters or numbers
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History:
From J.A. Mansour, jadmansour96(at)gmail.com
Acknowledgements:
The article is based on observations acquired with VISTA. The
observations were obtained as part of the VISTA Hemisphere Survey, ESO
Program, 179.A-2010 (PI: McMahon). The work of J.A.M. and part of the
work of M.P. was supported by a grant of the Romanian National
Authority for Scientific Research - UEFISCDI, project number
PN-III-P1-1.2-PCCDI-2017-0371. M.P., J.dL., and J.L. acknowledge
support from the AYA2015- 67772-R (MINECO, Spain). M.P. and J.dL. also
acknowledge financial support from projects SEV-2015-0548 and AYA2017-
89090-P (Spanish MINECO).
(End) Patricia Vannier [CDS] 21-Oct-2021