J/A+A/649/A111ivo://CDS.VizieR/J/A+A/649/A111doi:10.26093/cds/vizier.36490111CDSAdibekyan V.Santos N.C.Demangeon O.D.S.Faria J.P.Barros S.C.C.,Oshagh M.Figueira P.Delgado Mena E.Sousa S.G.Israelian G.,Campante T.Hakobyan A.A.2022-05-16T06:34:15Z2021-05-24T08:08:24ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsstellar-agesRevealing the mechanisms shaping the architecture of planetary systems is crucial for our understanding of their formation and evolution. In this context, it has been recently proposed that stellar clustering might be the key in shaping the orbital architecture of exoplanets. The main goal of this work is to explore the factors that shape the orbits of planets. We performed different statistical tests to compare the properties of planets and their host stars associated with different stellar environments. Results. We used a homogeneous sample of relatively young FGK dwarf stars with radial velocity detected planets and tested the hypothesis that their association to phase space (position-velocity) over-densities ("cluster" stars) and under-densities ("field" stars) impacts the orbital periods of planets. When controlling for the host star properties on a sample of 52 planets orbiting around cluster stars and 15 planets orbiting around field stars, we found no significant difference in the period distribution of planets orbiting these two populations of stars. By considering an extended sample of 73 planets orbiting around cluster stars and 25 planets orbiting field stars, a significant difference in the planetary period distributions emerged. However, the hosts associated with stellar under-densities appeared to be significantly older than their cluster counterparts. This does not allow us to conclude as to whether the planetary architecture is related to age, environment, or both. We further studied a sample of planets orbiting cluster stars to study the mechanism responsible for the shaping of orbits of planets in similar environments. We could not identify a parameter that can unambiguously be responsible for the orbital architecture of massive planets, perhaps, indicating the complexity of the issue. An increased number of planets in clusters and in over-density environments will help to build large and unbiased samples which will then allow to better understand the dominant processes shaping the orbits of planets.2021A&A...649A.111Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/649/A111CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/other/Nat/586.528 : Properties of exoplanet host stars (Winter+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/649/A111https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/649/A111http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/649/A111https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/649/A111https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/649/A111http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/649/A111GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/649/A111/ages (Ages of the planet host stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/649/A111/ages?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/649/A111/ages?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/649/A111/ages?GETtext/xml+votable180.050000true295.46655550.51752390.0055555555555555566/311 320 431 748 918 2110 2472 2497 3350 3876 4136 4429 4881 5067 5309 5522 6791 6821 7746 8357 9459 9483 9662 10079 12146 12465 12644 12983 13143 14278 14329 14412 14419 14548 14585 14682 14825 15131 15174 15345 16627 16652 16707 16995 17496 17641 17730 17954 18569 18614 18747 18821 19619 19904 19912 20145 20746 21473 21838 21906 22036 22252 22654 23030 23201 23414 23646 23681 24178 24312 24530 24831 25135 25593 25939 26183 26242 26706-26707 26790 26901 26978 26997 27018 27164 27616 28130 28571 28767 28779 29513 30015 30378 30526 30707 31494 31860 31874 32930 33042 33182 33243 33258 33430 33510 33630 33717 34069 34390 34674 34905 35339 35362 35442 35532 35839 35907 35954 36506 37018 37047 37461 37573 37954-37955 38545 38728 38998 39257 39280 39364 39646 40066 40220 40442 41058 41432 41446 41515 41724 41912 42205 42248 42318 42386 42510 42570 42760 43012 43228 43677 43775 43813 43818 43911 44223 44243 44740 45168 45364 45564 45717 45865 46111 46215 46297 46800 46843 46967 47550 47590 47780 48105 48178 48402 48519 48530https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/649/A111?format=asciidefaultJ/A+A/649/A111/agesAges of the planet host starsStarStar's identifiermeta.id;meta.maincharSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective TemperatureKphys.temperature.effectiveinte_TeffUncertainity of effective TemperatureKstat.error;phys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainity of surface gravitylog(cm.s**-2)stat.errorfloat[Fe/H]Iron abundance [Fe/H]log(Sun)phys.abund.Fefloate_[Fe/H]Uncertainity of iron abundance [Fe/H]log(Sun)stat.error;phys.abund.FefloatAgeIsochrone agesGyrtime.agefloate_AgeUncertainity of isochrone agesGyrstat.error;time.agefloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main