J/AJ/167/199ivo://CDS.VizieR/J/AJ/167/199doi:10.26093/cds/vizier.51670199CDSVissapragada S.Greklek-McKeon M.Linssen D.MacLeod M.,Thorngren D.P.Gao P.Knutson H.A.Latham D.W.Lopez-Morales M.,Oklopcic A.Gonzalez J.P.Saidel M.Tumborang A.Yoshida S.2024-11-06T20:19:51Z2024-08-19T09:33:01ZCDS support team

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

cds-question@unistra.frexoplanetsinfrared-astronomyspectroscopySuperpuffs are planets with exceptionally low densities ({rho}<~0.1g/cm^3^) and core masses (Mc<~5M{Earth}). Many lower-mass (Mp<~10M{Earth}) superpuffs are expected to be unstable to catastrophic mass loss via photoevaporation and/or boil-off, whereas the larger gravitational potentials of higher-mass (Mp>~10M{Earth}) superpuffs should make them more stable to these processes. We test this expectation by studying atmospheric loss in the warm, higher-mass superpuff TOI-1420b (M=25.1M{Earth}, R=11.9R{Earth}, {rho}=0.08g/cm^3^, Teq=960K). We observed one full transit and one partial transit of this planet using the metastable helium filter on Palomar/WIRC and found that the helium transits were 0.671%{+/-}0.079% (8.5{sigma}) deeper than the TESS transits, indicating an outflowing atmosphere. We modeled the excess helium absorption using a self-consistent 1D hydrodynamics code to constrain the thermal structure of the outflow given different assumptions for the stellar XUV spectrum. These calculations then informed a 3D simulation, which provided a good match to the observations with a modest planetary mass-loss rate of 1010.82g/s (Mp/M~70Gyr). Superpuffs with Mp>~10M{Earth}, like TOI-1420b and WASP-107b, appear perfectly capable of retaining atmospheres over long timescales; therefore, these planets may have formed with the unusually large envelope mass fractions they appear to possess today. Alternatively, tidal circularization could have plausibly heated and inflated these planets, which would bring their envelope mass fractions into better agreement with expectations from core-nucleated accretion.2024AJ....167..199Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/167/199CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)J/A+A/493/639 : Velocity curves of HD 40307 (Mayor+, 2009)J/ApJS/214/25 : Rosseland & Planck gaseous mean opacities (Freedman+, 2014)J/A+A/586/A75 : Simulations of hot gas planets atmospheres (Salz+, 2016)J/MNRAS/466/1868 : Neptune-like planets low-density overabund (Cubillos+ 2017)J/AJ/156/89 : RVs & predicted transit-times for K2-24 system (Petigura+, 2018)J/AJ/160/201 : Infrared transmission spectrum for Kepler-79d (Chachan+, 2020)J/AJ/159/57 : HST spectroscopic LCs of Kepler 51b & 51d (Libby-Roberts+, 2020)J/AJ/159/278 : He-filter observations WASP-69b & WASP-52b (Vissapragada+, 2020)J/AJ/161/70 : Radial velocities WASP-107 with HIRES & CORALIE (Piaulet+, 2021)J/AJ/161/119 : The TESS-Keck survey. IV. Rvel for WASP-107 (Rubenzahl+, 2021)J/AJ/165/48 : Transit times for Kepler-289 b, c and d (Greklek-McKeon+, 2023)J/AJ/166/181 : HARPS-N and NEID radial velocities of TOI-1420 (Yoshida+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/167/199https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/167/199http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/167/199https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/167/199https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/167/199http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/167/199GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/AJ/167/199/fig2The two phase-folded WIRC light curves of TOI-1420brecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDay[1/2] Day identifier (1)meta.id;meta.mainintTime[-0.18/0.2] Time from transit centerdtime.epochdoubleFlux[0.96/1.02] Relative fluxphot.flux;arith.ratiofloate_Flux[0.004/0.02] Uncertainty in Fluxstat.error;phot.fluxfloat