J/A+A/666/A116ivo://CDS.VizieR/J/A+A/666/A116doi:10.26093/cds/vizier.36660116CDSAthanasopoulos 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.2024-11-06T20:01:05Z2022-10-31T06:16:24ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frsolar-systemasteroidsFamilies 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) 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) as members of a 4 Gyr-old collisional family, have a common origin, thus strengthening their family membership.2022A&A...666A.116Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/666/A116CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/666/A116https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/666/A116http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/666/A116https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/666/A116https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/666/A116http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/666/A116GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/666/A116/tableb5Disk-integrated optical dense lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAstAsteroid number and namemeta.id;meta.maincharObs.dateThe date of the observations in the format: YYYY-MM-DD.D or YYYY.MM-YYYY.MM in case of TESStime.epoch;obscharNpThe number of individual measurementsmeta.numberintDelta? Asteroid's distance to the Earthaupos.distance;pos.geocentricfloatnullabler? Asteroid's distance to the Sunaupos.distance;pos.heliocentricfloatnullablephi? Asteroid's phase angledegsrc.orbitalfloatnullableFilterThe photometric filtermeta.id;instr.filtercharRefThe reference to the data (1)meta.ref;pos.framechar