J/A+A/674/A50ivo://CDS.VizieR/J/A+A/674/A50doi:10.26093/cds/vizier.36740050CDSDeshapriya J.D.P.Perna D.Bott N.Hasselmann P.H.Granvik M.Dotto E.,Fulchignoni M.Giunta A.Perozzi E.Ieva S.Petropoulou V.,Mazzotta Epifani E.2024-11-28T20:03:53Z2023-05-31T07:39:15ZCDS support team

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

cds-question@unistra.frasteroidsvisible-astronomyNear-Earth Objects (NEOs) are being discovered at an ever increasing rate. However, their physical characterisation significantly lags behind. In particular, the taxonomic classification of newly discovered NEOs is of great importance to better understand the population of NEOs. In this context, our goal is to probe potential links between orbital properties of NEOs and their composition. We investigate whether we can make a reasonable guess about the taxonomic class of an NEO upon its discovery with a decent orbital accuracy. We used G-mode multivariate statistical clustering method to find homogeneous clusters in a dataset composed of orbital elements of NEOs. We adopted two approaches using 2 sets of variables as inputs to the G-mode method. In each approach, we analysed the available taxonomic distribution of resulting clusters to find potential correlations with several unique parameters that distinctively characterise NEOs. We then applied a dynamical model on the same clusters to trace their escape regions. Approach 1 led us to obtain NEO clusters that can be linked to a primitive composition, and this result was further strengthened by the dynamical model, which mapped outer-belt sources as escape regions for these clusters. We remark the finding of a cluster akin to S-type NEOs in highly eccentric orbits during the same Approach 1. Two clusters: one with small NEOs in terrestrial-like orbits and one with relatively high inclinations were found to be common to both approaches. Approach 2 revealed three clusters only separable by their arguments of perihelion and, together they compose the majority of known Atira asteroids. For an NEO whose orbit is relatively well determined, we propose a model to determine whether the taxonomy of an NEO is siliceous or primitive if the orbital elements of the NEO fall within the presented combinations of inclination, eccentricity and semi-major axis ranges.2023A&A...674A..50Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A50CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+ 2014)https://www.minorplanetcenter.net/iau/mpc.html : MPC Home Pagehttps://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/ : SBDB Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/674/A50https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/674/A50http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/674/A50https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/674/A50https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/674/A50http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/674/A50GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/674/A50/datasetData of NEOs that were used to obtain the results of this paperNumber? NEO numbermeta.idintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDesignNEO designation (0 for none)meta.id;meta.maincharUnc[0/5] MPC "U" parameter which gives the uncertainty of the orbit of the NEO (1)meta.codeintorbitType[1/4] Dynamical orbital type (2)meta.codeintiNEO orbit inclination (the angle with respect to x-y ecliptic plane)degsrc.orbital.inclinationdoubleeNEO orbit eccentricitysrc.orbital.eccentricitydoubleaNEO orbit semi-major axisauphys.angSize.smajAxisdoubleqNEO orbit perihelionausrc.orbital.periastrondoubleQNEO orbit aphelionaupos.distance;src.orbitaldoubleeMOIDMinimum orbit intersection distance with respect to Earthaupos.distance;src.orbitaldoubleTaxoNEO taxonomic classmeta.code.classcharHNEO absolute magnitudemagphys.magAbsdoubleTJTisserand Parameter of the NEO with respect to Jupitersrc.orbitaldoubleAlbedo? Geometric albedo of the NEO%phys.albedodoublenullableomegaArgument of the perihelion of the NEOdegsrc.orbital.periastrondoubleNameNEO name (0 for none)meta.idchar