J/A+A/616/A151ivo://CDS.VizieR/J/A+A/616/A151doi:10.26093/cds/vizier.36160151CDSCasasayas-Barris N.Palle E.Yan F.Chen G.Albrecht S.Nortmann L.,Van Eylen V.Snellen I.Talens G.J.J.Gonzalez Hernandez J.I.,Rebolo R.Otten G.P.P.L.2018-09-28T08:32:57Z2018-09-07T07:32:06ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsspectroscopyWe used the HARPS-North high resolution spectrograph (R=115000) at Telescopio Nazionale Galileo (TNG) to observe one transit of the highly irradiated planet MASCARA-2b/KELT-20b. Using only one transit observation, we are able to clearly resolve the spectral features of the atomic sodium (NaI) doublet and the H{alpha} line in its atmosphere, which are corroborated with the transmission calculated from their respective transmission light curves (TLC). In particular, we resolve two spectral features centred on the NaI doublet position with an averaged absorption depth of 0.17+/-0.03% for a 0.75{AA} bandwidth with line contrasts of 0.44+/-0.11% (D2) and 0.37+/-0.08% (D1). The NaI TLC have also been computed, showing a large Rossiter-McLaughlin (RM) effect, which has a 0.20+/-0.05% NaI transit absorption for a 0.75{AA} passband that is consistent with the absorption depth value measured from the final transmission spectrum. We observe a second feature centred on the H{alpha} line with 0.6+/-0.1% contrast and an absorption depth of 0.59+/-0.08% for a 0.75{AA} passband that has consistent absorptions in its TLC, which corresponds to an effective radius of R'/Rp=1.20+/-0.04. While the signal-to-noise ratio (S/N) of the final transmission spectrum is not sufficient to adjust different temperature profiles to the lines, we find that higher temperatures than the equilibrium (Teq=2260+/-50K) are needed to explain the lines contrast. Particularly, we find that the NaI lines core require a temperature of T=4210+/-180K and that H{alpha} requires a temperature of T=4330+/-520K. MASCARA-2b, like other planets orbiting A-type stars, receives a large amount of UV energy from its host star. This energy excites the atomic hydrogen and produces H{alpha} absorption, leading to the expansion and abrasion of the atmosphere. The study of other Balmer lines in the transmission spectrum would allow the determination of the atmospheric temperature profile and the calculation of the lifetime of the atmosphere with escape rate measurements. In the case of MASCARA-2b, residual features are observed in the H{beta} and H{gamma} lines, but they are not statistically significant.More transit observations are needed to confirm our findings in NaI and H{alpha} and to build up enough S/N to explore the presence of H{beta} and H{gamma} planetary absorptions.2018A&A...616A.151Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/616/A151CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/612/A57 : MASCARA-2 b (HD185603) light curves and spectra (Talens+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/616/A151https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/616/A151http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/616/A151https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/616/A151https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/616/A151http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/616/A151GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/616/A151/lcm2bhaTransmission light curves around H{alpha}PhaseOrbital phasetime.phasedoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFlux300Relative Flux in a 3.00 Angstrom passband (1)phot.flux;arith.ratiodoublee_Flux300Errors for a 3.00A passbandstat.errordoubleFlux500Relative Flux in a 5.00 Angstrom passband (1)phot.flux;arith.ratiodoublee_Flux500Errors for a 5.00A passbandstat.errordoubleFlux1000Relative Flux in a 10.0 Angstrom passband (1)phot.flux;arith.ratiodoublee_Flux1000Errors for a 10.0A passbandstat.errordoubleFlux2000Relative Flux in a 20.0 Angstrom passband (1)phot.flux;arith.ratiodoublee_Flux2000Errors for a 20.0A passbandstat.errordoubleJ/A+A/616/A151/tsm2bnaTransmission spectrum around NarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength in Angstroem0.1nmem.wlfloatFluxRelative Flux in % (1)%phot.flux;arith.ratiodoublee_FluxError in relative flux%stat.error;phot.fluxdoubleJ/A+A/616/A151/lcm2bnaTransmission light curves around NarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhaseOrbital phasetime.phasedoubleFlux075Relative Flux in a 0.75 Angstroem passband (1)phot.flux;arith.ratiodoublee_Flux075Errors for a 0.75A passbandstat.errordoubleFlux150Relative Flux in a 1.50 Angstroem passband (1)phot.flux;arith.ratiodoublee_Flux150Errors for a 1.50A passbandstat.errordoubleFlux300Relative Flux in a 3.0 Angstroem passband (1)phot.flux;arith.ratiodoublee_Flux300Errors for a 3.0A passbandstat.errordoubleFlux500Relative Flux in a 5.0 Angstroem passband (1)phot.flux;arith.ratiodoublee_Flux500Errors for a 5.0A passbandstat.errordoubleJ/A+A/616/A151/tsm2bhaTransmission spectrum around H{alpha}recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength in Angstroem0.1nmem.wlfloatFluxRelative Flux in % (1)%phot.flux;arith.ratiodoublee_FluxError in relative flux%stat.error;phot.fluxdouble