J/A+A/668/A29ivo://CDS.VizieR/J/A+A/668/A29doi:10.26093/cds/vizier.36680029CDSGrieves N.Bouchy F.Ulmer-Moll S.Gill S.Anderson D.R.Psaridi A.,Lendl M.Stassun K.G.Jenkins J.M.Burleigh M.R.Acton J.S.Boyd P.T.,Casewell S.L.Eigmueller P.Goad M.R.Goeke R.F.Guenther M.N.,Hawthorn F.Henderson B.A.Henze C.E.Jordan A.Kendall A.Mishra L.,Moldovan D.Moyano M.Osborn H.Revol A.Sefako R.R.Tilbrook R.H.,Udry S.Unger N.Vines J.I.West R.G.Worters H.L.2024-11-06T20:01:45Z2022-12-02T09:33:00ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsphotometryvisible-astronomyWe report the discovery of a 1.32^+0.10^_-0.10_M_Jup_ planet orbiting on a 75.12 day period around the G3V 10.8^+2.1^_-3.6_Gyr old star TOI-5542 (TIC 466206508; TYC 9086-1210-1). The planet was first detected by the Transiting Exoplanet Survey Satellite (TESS) as a single transit event in TESS Sector 13. A second transit was observed 376 days later in TESS Sector 27. The planetary nature of the object has been confirmed by ground-based spectroscopic and radial velocity observations from the CORALIE and HARPS spectrographs. A third transit event was detected by the ground-based facilities NGTS, EulerCam, and SAAO. We find the planet has a radius of 1.009^+0.036^_-0.035_R_Jup_ and an insolation of 9.6^+0.9^_-0.8_S_{sun}_, along with a circular orbit that most likely formed via disk migration or in situ formation, rather than high-eccentricity migration mechanisms. Our analysis of the HARPS spectra yields a host star metallicity of [Fe/H]=-0.21+/-0.08, which does not follow the traditional trend of high host star metallicity for giant planets and does not bolster studies suggesting a difference among low- and high-mass giant planet host star metallicities. Additionally, when analyzing a sample of 216 well-characterized giant planets, we find that both high masses (4M_Jup_<M_p_<13M_Jup_) and low masses (0.5M_Jup_<M_p_<4M_Jup_), as well as both both warm (P>10-days) and hot (P<10-days) giant planets are preferentially located around metal-rich stars (mean [Fe/H]>0.1). TOI-5542b is one of the oldest known warm Jupiters and it is cool enough to be unaffected by inflation due to stellar incident flux, making it a valuable contribution in the context of planetary composition and formation studies.2022A&A...668A..29Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A29CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/668/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/668/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/668/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/668/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/668/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/668/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/668/A29/saaoSAAO photometryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Date (BJD) in the Barycentric Dynamical Time (TDB) standarddtime.epochdoubleAirmassAirmassobs.airMassdoubleFWHMTarget FWHMarcsecspect.line.widthdoubleSkySky backgroundmeta.notefloatExpTimeExposure timestime.duration;obs.exposurefloatFluxRelative Fluxphot.flux;arith.ratiodoublee_FluxRelative Flux errorstat.error;phot.fluxdoublexshiftTarget x position shiftpixpos.cartesian.x;instr.detfloatyshiftTarget y position shiftpixpos.cartesian.y;instr.detfloatJ/A+A/668/A29/ecamEulerCam photometryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Date (BJD) in the Barycentric Dynamical Time (TDB) standarddtime.epochdoubleFluxRelative Fluxphot.flux;arith.ratiodoublee_FluxRelative Flux errorstat.error;phot.fluxdoublexshiftTarget x position shiftpixpos.cartesian.x;instr.detfloatyshiftTarget y position shiftpixpos.cartesian.y;instr.detfloatAirmassAirmassobs.airMassdoubleFWHMTarget FWHMarcsecspect.line.widthdoubleSkySky backgroundmeta.notefloatExpTimeExposure timestime.duration;obs.exposurefloat