Properties of exoplanet host stars J/other/Nat/586. ivo://CDS.VizieR/J/other/Nat/586.528 CDS Winter A.J. Kruijssen J.M.D. Longmore S.N. Chevance M. 2021-09-09T09:04:37Z 2020-11-20T10:29:15Z CDS support team CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France cds-question@unistra.fr multiple-stars exoplanets stellar-masses stellar-ages Planet formation is generally described in terms of a system containing the host star and a protoplanetary disk, of which the internal properties (for example, mass and metallicity) determine the properties of the resulting planetary system. However, (proto)planetary systems are predicted and observed to be affected by the spatially clustered stellar formation environment, through either dynamical star-star interactions or external photoevaporation by nearby massive stars. It is challenging to quantify how the architecture of planetary sysems is affected by these environmental processes, because stellar groups spatially disperse within less than a billion years, well below the ages of most known exoplanets. Here we identify old, co-moving stellar groups around exoplanet host stars in the astrometric data from the Gaia satellite and demonstrate that the architecture of planetary systems exhibits a strong dependence on local stellar clustering in position-velocity phase space. After controlling for host stellar age, mass, metallicity and distance from the star, we obtain highly significant differences (with p values of 10^-5^ to 10^-2^) in planetary system properties between phase space overdensities (composed of a greater number of co-moving stars than unstructured space) and the field. The median semi-major axis and orbital period of planets in phase space overdensities are 0.087 astronomical units and 9.6 days, respectively, compared to 0.81 astronomical units and 154 days, respectively, for planets around field stars. 'Hot Jupiters' (massive, short-period exoplanets) predominantly exist in stellar phase space overdensities, strongly suggesting that their extreme orbits originate from environmental perturbations rather than internal migration or planet-planet scattering. Our findings reveal that stellar clustering is a key factor setting the architectures of planetary systems. 2020Natur.586..528W https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/Nat/586.528 Catalog Research IsServedBy TAP VizieR generic service IsServedBy Conesearch service related-to I/345 : Gaia DR2 (Gaia Collaboration, 2018) https://cds.unistra.fr/vizier-org/licences_vizier.html https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/other/Nat/586.528 https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/other/Nat/586.528 http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/other/Nat/586.528 https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/other/Nat/586.528 https://vizier.iucaa.in/viz-bin/votable?-source=J/other/Nat/586.528 http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/other/Nat/586.528 GET text/xml+votable https://tapvizier.cds.unistra.fr/TAPVizieR/tap Cone search capability for table J/other/Nat/586.528/table1 (Properties of exoplanet host stars with six-dimensional astrometric data from Gaia DR2) https://vizier.cds.unistra.fr/viz-bin/conesearch/J/other/Nat/586.528/table1? https://vizier.iucaa.in/viz-bin/conesearch/J/other/Nat/586.528/table1? http://vizieridia.saao.ac.za/viz-bin/conesearch/J/other/Nat/586.528/table1? 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https://cdsarc.cds.unistra.fr/viz-bin/moc/J/other/Nat/586.528?format=ascii default J/other/Nat/586.528/table1 Properties of exoplanet host stars with six-dimensional astrometric data from Gaia DR2 recno Record number assigned by the VizieR team. Should Not be used for identification. meta.record int Host Exoplanet host star meta.note char M* ? Stellar mass (1) solMass phys.mass float nullable e_M* ? Stellar mass error (1) solMass stat.error float nullable Tage ? Age (1) Gyr time.age float nullable e_Tage ? Age error (1) Gyr stat.error float nullable S Number of neighbouring stars within 40pc used to construct the relative phase space density distribution meta.number int logPnull Probability the local phase space densities are consistent with a single lognormal distribution stat.fit.goodness float BIC1-2 Difference between the Bayesian information criterion (BIC) of the one-component lognormal fit to the phase space density distribution and the two-component fit stat.fit.param float logbetaM20 Relative phase space density stat.fit.param float logPhigh Probability that the star occupies a phase space overdensity stat.fit.goodness float HJ? [Y/N] whether the star is orbited by a hot Jupiter meta.code char Include? [Y/N] whether it is included in the final sample after applying our selection cuts meta.code char SimbadName Simbad column added by the CDS meta.id char _RA Right Ascension (J2000) from SIMBAD (not part of the original data) deg pos.eq.ra;meta.main nullable _DE Declination (J2000) from SIMBAD (not part of the original data) deg pos.eq.dec;meta.main nullable