J/A+A/666/A116 Asteroid spin-states of 4 Gyr-old family (Athanasopoulos+, 2022)
Asteroid spin-states of a 4 Gyr-old collisional family.
Athanasopoulos D., Hanus J., Avdellidou C., Bonamico R., Delbo M.,
Conjat M., Ferrero A., Gazeas K., Rivet J.P., Sioulas N., van Belle G.,
Antonini P., Audejean M., Behrend R., Bernasconi L., Brinsfield J.W.,
Brouillard S., Brunetto L., Fauvaud M., Fauvaud S., Gonzalez R., Higgins D.,
Holoien T.W.-S., Kobber G., Koff R.A., Kryszczynska A., Livet F.,
Marciniak A., Oey J., Pejcha O., Rives J.J., Roy R.
<Astron. Astrophys. 666, A116 (2022)>
=2022A&A...666A.116A 2022A&A...666A.116A (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets
Keywords: minor planets - asteroids: general -
astronomical databases: miscellaneous
Abstract:
Families of asteroids generated by the collisional fragmentation of a
common parent body have been identified using clustering methods of
asteroids in their proper orbital element space. However, there is
growing evidence that some of the real families are larger than the
corresponding cluster of objects in orbital elements, as well as there
are families that escaped identification from clustering methods. An
alternative method has been developed in order to identify collisional
families from the correlation between the asteroid fragment sizes and
their proper semimajor axis distance from the family center (V-shape).
This method has been shown to be effective in the cases of the very
diffuse families that formed Gyrs ago. Here we use multiple technique
observations of asteroids to provide corroborating evidence that one
of those groups of asteroids identified as a family from the
correlation between size and proper semimajor axis of asteroids are
real fragments of a common parent body and, thus form a collisional
family. We obtained photometric observations of asteroids in order to
construct their rotational lightcurves, we combine these with
literature lightcurves and sparse-in-time photometry, we input these
data in the so-called lightcurve inversion methods, which allow us to
determine a convex approximation to the 3D shape of the asteroids and
their orientation in space; from the latter we extract the latitude
(or obliquity) of the spin pole in order to assess whether an object
is prograde or retrograde. We included in the analysis spin pole
solutions already published in the literature aiming to increase the
statistical significance of our results. The ultimate goal is to
assess whether we find an excess on retrograde asteroids in the inward
side of the V-shape of a 4-Gyr old asteroid family identified by Delbo
et al. (2017Sci...357.1026D 2017Sci...357.1026D) with the V-shape method. This excess of
retrograde rotators is predicted by the theory of asteroid family
evolution. We obtained the latitude of the spin poles for 55 asteroids
claimed to belong to a 4 Gyr-old collisional family of the inner main
belt that consists of low-albedo asteroids. After having re-evaluated
the albedo and spectroscopic information, we found that nine of the
aforementioned asteroids are interlopers in the 4 Gyr-old family. Of
the 46 remaining asteroids, 31 are found to be retrograde, whereas 15
prograde. We also found that this excess of retrograde rotators have
very low probability (1.29%) to be due to random sampling from an
underling uniform distribution of spin poles. Our results constitute a
corroborating evidence that the asteroids identified by Delbo et al.
(2017Sci...357.1026D 2017Sci...357.1026D) as members of a 4 Gyr-old collisional family,
have a common origin, thus strengthening their family membership.
Description:
Disk-integrated optical dense lightcurves utilized for the physical
characterization of primordial family asteroids.
The table is separated into 37 blocks, each one corresponds to an
asteroid.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb5.dat 116 444 Disk-integrated optical dense lightcurves
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 A22 --- Ast Asteroid number and name
24- 38 A15 --- Obs.date The date of the observations in the format:
YYYY-MM-DD.D or YYYY.MM-YYYY.MM
in case of TESS
46- 49 I4 --- Np The number of individual measurements
51- 54 F4.2 au Delta ? Asteroid's distance to the Earth
56- 59 F4.2 au r ? Asteroid's distance to the Sun
61- 64 F4.1 deg phi ? Asteroid's phase angle
66- 67 A2 --- Filter The photometric filter
69-116 A48 --- Ref The reference to the data (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
Baker2010 = Baker R.E., Benishek V., Pilcher F. & Higgins D.
2010, Minor Planet Bulletin, 37, 81
Benishek2017 = Benishek V. 2017, Minor Planet Bulletin, 44, 67
Benishek2020 = Benishek V. 2020, Minor Planet Bulletin, 47, 75
Binzel1983 = Binzel R.P. & Mulholland, J. D. 1983, Icarus, 56, 519
Binzel1987a = Binzel R.P. 1987, Icarus, 72, 135
Binzel1992b = Binzel R.P., Xu S., Bus S.J. & Bowell E.
1992, Icarus, 99, 225
Buchheim2007 = Buchheim R.K. 2007, Minor Planet Bulletin, 34, 68
Carreno2019 = Carreno A., Arce E., Fornas G. & Mas V.
2019, Minor Planet Bulletin, 46, 200
Hanus2016a = Hanus J., Durech J., Oszkiewicz D.A., et al.
2016A&A...586A.108H 2016A&A...586A.108H
Higgins2008 = Higgins D. 2008, Minor Planet Bulletin, 35, 30
Higgins2011a = Higgins D. 2011, Minor Planet Bulletin, 38, 41
Klinglesmith2017 = Klinglesmith Daniel A.I.
2017, Minor Planet Bulletin, 44, 127
Kryszczynska2012 = Kryszczynska A., Colas F., Polinska M. et al.
2012A&A...546A..72K 2012A&A...546A..72K, Cat. J/A+A/546/A72
Mohamed1994 = Mohamed R.A., Chiorny V.G., Dovgopol A.N. &
Shevchenko V.G. 1994A&AS..108...69M 1994A&AS..108...69M
Pilcher2015b = Pilcher F. 2015, Minor Planet Bulletin, 42, 190
Pray2010 = Pray D.P. & Durkee R.I.
2010, Minor Planet Bulletin, 37, 35
Skiff2019 = Skiff B.A., McLelland K.P., Sanborn J.J., Pravec P. &
Koehn B.W. 2019, Minor Planet Bulletin, 46, 238
Stephens2010b = Stephens R.D. & Warner B.D.
2010, Minor Planet Bulletin, 37, 124
Stephens2011a = Stephens R.D. 2011, Minor Planet Bulletin, 38, 23
Stephens2019b = Stephens R.D. & Warner B.D.
2019b, Minor Planet Bulletin, 46, 449
Stephens2020c = Stephens R.D. & Warner B.D.
2020, Minor Planet Bulletin, 47, 224
Strabla2011 = Strabla L., Quadri U. & Girelli R.
2011, Minor Planet Bulletin, 38, 169
Warner2004b = Warner B.D. 2004, Minor Planet Bulletin, 31, 36
Warner2006 = Warner B.D. 2006, Minor Planet Bulletin, 33, 58
Warner2010c = Warner B.D. 2010, Minor Planet Bulletin, 37, 161
Warner2014 = Warner B.D. 2014, Minor Planet Bulletin, 41, 144
Wisniewski1997 = Wisniewski W.Z., Michalowski T.M., Harris A.W. &
McMillan R.S. 1997, Icarus, 126, 395
--------------------------------------------------------------------------------
Acknowledgements:
Dimitrios Athanasopolos, dimathanaso(at)phys.uoa.gr
Josef Hanus, josef.hanus(at)mff.cuni.cz
(End) Patricia Vannier [CDS] 08-Jul-2022