J/A+A/689/A250ivo://CDS.VizieR/J/A+A/689/A250doi:10.26093/cds/vizier.36890250CDSCastro-Gonzalez A.Bourrier V.Lillo-Box J.Delisle J.-B.,Armstrong D.J.Barrado D.Correia A.C.M.2025-02-24T20:01:00Z2024-09-17T12:29:06ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsvisible-astronomyAtmospheric and dynamical processes are thought to play a major role in shaping the distribution of close-in exoplanets. A striking feature of such distribution is the Neptunian desert, a dearth of Neptunes on the shortest-period orbits. We aim at delineating the Neptunian desert boundaries and studying its transition into the savanna, a moderately populated region at larger orbital distances. This will allow bringing constraints to the processes that carved out the Neptunian landscape and provide the exoplanet community with a framework to perform studies of planet formation and evolution. We built a sample of planets and candidates based on the Kepler DR25 catalogue and weighed it according to the transit and detection probabilities. We used the corrected distribution to study occurrences across the period and period-radius spaces. We delimited the Neptunian desert as the close-in region of the period-radius space with no planets at a 3{sigma} level, and provide the community with simple, ready-to-use approximate boundaries. We identified an overdensity of planets separating the Neptunian desert and savanna (3.2d<~ P_orb_<~5.7d) that stands out at a 4.7{sigma} level above the desert and at a 3.5{sigma} level above the savanna, which we propose to call the Neptunian ridge. The period range of the ridge matches that of the well-known hot Jupiter pileup (~=3-5 days), which suggests that similar evolutionary processes might act on both populations. We find that the occurrence fraction between the pileup and warm Jupiters (f_pileup/warm_=5.3+/-1.1) is about twice that between the Neptunian ridge and savanna (f_ridge/savanna_=2.7+/-0.5). This indicates either that the processes that drive or maintain planets in the overdensity are more efficient for Jupiters or that the processes that drive or maintain planets in the warm region are more efficient for Neptunes. Our revised landscape supports a previous hypothesis that a fraction of Neptunes were brought to the edge of the desert (i.e. the newly identified ridge) through high-eccentricity tidal migration (HEM) late in their life, surviving the evaporation that eroded Neptunes that arrived earlier on in the desert. The ridge thus appears as a true physical feature illustrating the interplay between photoevaporation and HEM processes, providing further evidence of their role in shaping the distribution of close-in Neptunes.2024A&A...689A.250Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/689/A250CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/133 : Kepler Input Catalog (Kepler Mission Team, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/689/A250https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/689/A250http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/689/A250https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/689/A250https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/689/A250http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/689/A250GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/689/A250/table1 (Transit and detection probabilities of the Kepler DR25 catalogue)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/689/A250/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/689/A250/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/689/A250/table1?GETtext/xml+votable180.050000true286.8084949.31641420.0055555555555555564/922-923 933-935 944-946 5/3645-3647 3683 3704 3706 3729-3731 3788-3789 3792-3793 6/14567 14573 14575 14577-14579 14730-14731 14738 14744 14746 14749-14751 14792 14794-14795 14828 14830 14914-14915 15040-15041 15043-15045 15057 15059-15062 15160-15161 15176 15178 15200 15232-15233https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/689/A250?format=asciiOpticaldefaultJ/A+A/689/A250/table1Transit and detection probabilities of the Kepler DR25 catalogueSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintKOIKepler Object of Interestmeta.notechar1/ptransitInverse of the transit probabilitystat.fit.goodnessdouble1/pdetectionInverse of the detection probabilitystat.fit.goodnessdoubleWeightAssigned weight to correct for non-transiting orbital inclinations and insufficient photometric precisionstat.weight;phys.atmol.weightdouble_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