J/A+A/684/A22ivo://CDS.VizieR/J/A+A/684/A22doi:10.26093/cds/vizier.36840022CDSPassegger V.M.Suarez Mascareno A.Allart R.Gonzalez Hernandez J.I.,Lovis C.Lavie B.Silva A.M.Mueller H.M.Tabernero H.M.Cristiani S.,Pepe F.Rebolo R.Santos N.C.Adibekyan V.Alibert Y.,Allende Prieto C.Barros S.C.C.Bouchy F.Castro-Gonzalez A.,D'Odorico V.Dumusque X.Di Marcantonio P.Ehrenreich D.Figueira P.,Genova Santos R.Lo Curto G.Martins C.J.A.P.Mehner A.Micela G.,Molaro P.Nari N.Nunes N.J.Palle E.Poretti E.Rodrigues J.,Sousa S.G.Sozzetti A.Udry S.Zapatero Osorio M.R.2024-11-07T20:02:41Z2024-04-03T09:23:01ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsradial-velocityvisible-astronomyDeriving metallicities for solar-like stars follows well-established GJ 9827 is a bright, nearby K7V star orbited by two super-Earths and one mini-Neptune on close-in orbits. The system was first discovered using K2 data and then further characterized by other spectroscopic and photometric instruments. Previous literature studies provide several mass measurements for the three planets, however, with large variations and uncertainties. To better constrain the planetary masses, we added high-precision radial velocity measurements from ESPRESSO to published datasets from HARPS, HARPS-N, and HIRES and we performed a Gaussian process analysis combining radial velocity and photometric datasets from K2 and TESS. This method allowed us to model the stellar activity signal and derive precise planetary parameters. We determined planetary masses of Mb=4.28^+0.35^_-0.33_M_{Earth}_, Mc=1.86^+0.37^_-0.39_M_{Earth}_, and Md=3.02^+0.58^_-0.57_M_{Earth}_, and orbital periods of 1.208974+/-0.000001 days for planet b, 3.648103^+0.000013^_-0.000010_ days for planet c, and 6.201812+/-0.000009 days for planet d. We compared our results to literature values and found that our derived uncertainties for the planetary mass, period, and radial velocity amplitude are smaller than the previously determined uncertainties. We modeled the interior composition of the three planets using the machine-learning-based tool ExoMDN and conclude that GJ 9827 b and c have an Earth-like composition, whereas GJ 9827 d has an hydrogen envelope, which, together with its density, places it in the mini-Neptune regime.2024A&A...684A..22Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/684/A22CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/484/3731 : GJ 9827 HARPS-N RV data (Rice+, 2019)J/AJ/161/47 : RV and photometry of HD106315 and GJ9827 (Kosiarek+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/684/A22https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/684/A22http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/684/A22https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/684/A22https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/684/A22http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/684/A22GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/684/A22/espressoS-BART extracted RVs from ESPRESSOrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Datedtime.epochdoubleRVRadial velocitykm/sphys.veloc;pos.heliocentricdoublee_RVError in radial velocitykm/sstat.errordoubleJ/A+A/684/A22/harpsS-BART extracted RVs from HARPSrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Datedtime.epochdoubleRVRadial velocitykm/sphys.veloc;pos.heliocentricdoublee_RVError in radial velocitykm/sstat.errordouble