J/A+A/647/A180ivo://CDS.VizieR/J/A+A/647/A180doi:10.26093/cds/vizier.36470180CDSGrieves N.Nielsen L.D.Vines J.I.Bryant E.M.Gill S.Bouchy F.,Lendl M.Bayliss D.Eigmueller P.Segransan D.Acton J.S.,Anderson D.R.Burleigh M.R.Casewell S.L.Chaushev A.Cooke B.F.,Gillen E.Goad M.R.Guenther M.N.Henderson B.A.Hogan A.Jenkins J.S.,Alves D.R.Jordan A.McCormac J.Moyano M.Queloz D.Raynard L.,Seidel J.V.Smith A.M.S.Tilbrook R.H.Udry S.West R.G.Wheatley P.J.2021-09-16T11:55:08Z2021-03-31T07:47:32ZCDS 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 the massive hot Jupiter NGTS-13b by the Next Generation Transit Survey (NGTS). The V=12.7 host star is likely in the subgiant evolutionary phase with logg_*_=4.04+/-0.05, Teff=5819+/-73K, M_*_=1.30^+0.11^_-0.18_M_{sun}_, and R_*_=1.79+/-0.06R_{sun}_. NGTS detected a transiting planet with a period of P=4.12 days around the star, which was later validated with the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame image photometry combined with CORALIE radial velocities we determine NGTS-13b to have a radius of R_P_=1.142+/-0.046R_Jup_, mass of M_P_=4.84+/-0.44M_Jup_ and eccentricity e=0.086+/-0.034. Some previous studies suggest that ~4M_Jup_ may be a border between two separate formation scenarios (e.g., core accretion and disk instability) and that massive giant planets share similar formation mechanisms as lower-mass brown dwarfs. NGTS-13b is just above 4M_Jup_ making it an important addition to the statistical sample needed to understand the differences between various classes of substellar companions. The high metallicity, [Fe/H]=0.25+/-0.17, of NGTS-13 does not support previous suggestions that massive giants are found preferentially around lower metallicity host stars, but NGTS-13b does support findings that more massive and evolved hosts may have a higher occurrence of close-in massive planets than lower-mass unevolved stars.2021A&A...647A.180Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/647/A180CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/647/A180https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/647/A180http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/647/A180https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/647/A180https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/647/A180http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/647/A180GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/647/A180/ngtsReduced NGTS photometry of NGTS-13recnoRecord 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.fluxdoubleJ/A+A/647/A180/tessReduced TESS photometry of NGTS-13recnoRecord 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.fluxdouble