J/ApJ/899/29ivo://CDS.VizieR/J/ApJ/899/29doi:10.26093/cds/vizier.18990029CDSKanodia S.Canas C.I.Stefansson G.Ninan J.P.Hebb L.Lin A.S.J.,Baran H.Maney M.Terrien R.C.Mahadevan S.Cochran W.D.Endl M.,Dong J.Bender C.F.Diddams S.A.Ford E.B.Fredrick C.Halverson S.,Hearty F.Metcalf A.J.Monson A.Ramsey L.W.Robertson P.Roy A.,Schwab C.Wright J.T.2022-03-14T09:03:00Z2021-10-28T08:33:19ZCDS support team

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

cds-question@unistra.frexoplanetsm-starsdwarf-starsinfrared-photometryvisible-astronomyphotometryradial-velocityWe confirm the planetary nature of TOI-1728b using a combination of ground-based photometry, near-infrared Doppler velocimetry and spectroscopy with the Habitable-zone Planet Finder. TOI-1728 is an old, inactive M0 star with Teff=3980_-32_^+31^K, which hosts a transiting super-Neptune at an orbital period of ~3.49days. Joint fitting of the radial velocities and TESS and ground-based transits yields a planetary radius of 5.05_-0.17_^+0.16^ R{Earth}, mass 26.78_-5.13_^+5.43^M{Earth}, and eccentricity 0.057_-0.039_^+0.054^. We estimate the stellar properties, and perform a search for He 10830{AA} absorption during the transit of this planet and claim a null detection with an upper limit of 1.1% with 90% confidence. A deeper level of He 10830{AA} absorption has been detected in the planet atmosphere of GJ3470b, a comparable gaseous planet. TOI-1728b is the largest super-Neptune-the intermediate subclass of planets between Neptune and the more massive gas-giant planets-discovered around an M-dwarf. With its relatively large mass and radius, TOI-1728 represents a valuable data point in the M-dwarf exoplanet mass-radius diagram, bridging the gap between the lighter Neptune-sized planets and the heavier Jovian planets known to orbit M dwarfs. With a low bulk density of 1.14_-0.24_^+0.26^g/cm^3^, and orbiting a bright host star (J~9.6, V~12.4), TOI-1728b is also a promising candidate for transmission spectroscopy both from the ground and from space, which can be used to constrain planet formation and evolutionary models.2020ApJ...899...29Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/899/29CatalogResearchIsServedByTAP VizieR generic servicerelated-toIV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)J/A+A/624/A49 : Spectra Earth-like planets around M-dwarfs (Wunderlich+, 2019)J/AJ/157/113 : TESS M-dwarf exoplanetary systems (Ballard, 2019)J/ApJ/887/261 : Compilation planets around M dwarfs (Martinez-Rodriguez+, 2019)J/AJ/159/100 : Flux & RVs of the dwarf G9-40 with K2 & HPF (Stefansson+, 2020)J/AJ/160/192 : Photometry and RVs of K2-25b with HPF (Stefansson+, 2020)J/AJ/160/259 : HPF RVs and TESS photometry of TOI-1266 (Stefansson+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/899/29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/899/29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/899/29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/899/29https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/899/29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/899/29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/ApJ/899/29/table1RVs of TOI-1728recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[0/35] Observation sequence numbermeta.id;meta.mainintBJD[2458907/2458960] Barycentric Julian Datedtime.epochdoubleRVel[-38.93/42.74] Radial Velocitym/sphys.veloc;pos.heliocentricfloate_RVel[7.34/32.39] Uncertainty in RVelm/sstat.error;spect.dopplerVelocfloatSNR[42/175] Signal-to-noise ratiostat.snrintJ/ApJ/899/29/fig9Posteriors from dynamic nested sampling from julietrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[0/45007] Sequential running numbermeta.id;meta.mainintPer[3.4912/3.4918] Orbital Perioddtime.perioddoubleRp/R*[0.06/0.09] Scaled Radiusphys.size;arith.ratiodoublea/R*[12.6/14.3] Scaled Semi-major axisphys.size.axisRatiodoubleb[0.0003/0.75] Impact Parametersrc.impactParamdoubleecoso[-0.61/0.52] e-omega parameterization, sqrt(e)*cosine({omega})src.orbital.eccentricitydoubleesino[-0.53/0.41] e-omega parameterization, sqrt(e)*sine({omega})src.orbital.eccentricitydoubleD-TESS[0.067/1] Dilution due to presence of background stars in TESS apertureinstr.backgrounddoubleK[0.49/35.5] RVel semi-amplitudem/sphys.veloc;src.orbitaldouble