J/A+A/538/A46ivo://CDS.VizieR/J/A+A/538/A46doi:10.26093/cds/vizier.35380046CDSde Mooij E.J.W.Brogi M.de Kok R.J.Koppenhoefer J.Nefs S.V.,Snellen I.A.G.Greiner J.Hanse J.Heinsbroek R.C.Lee C.H.,van der Werf P.P.2017-07-11T13:08:31Z2012-01-31T09:04:30ZCDS support team

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

cds-question@unistra.frmultiple-starssolar-system-planetsinfrared-photometryGJ1214b, the 6.55 Earth-mass transiting planet recently discovered by the MEarth team, has a mean density of 35% of that of the Earth. It is thought that this planet is either a mini-Neptune, consisting of a rocky core with a thick, hydrogen-rich atmosphere, or a planet with a composition dominated by water. In the case of a hydrogen-rich atmosphere, molecular absorption and scattering processes may result in detectable radius variations as a function of wavelength. The aim of this paper is to measure these variations. We have obtained observations of the transit of GJ1214b in the r- and I-band with the Isaac Newton Telescope (INT), in the g-, r-, i- and z-bands with the 2.2m MPI/ESO telescope, in the Ks-band with the Nordic Optical Telescope (NOT), and in the Kc-band with the William Herschel Telescope (WHT). By comparing the transit depth between the the different bands, which is a measure for the planet-to-star size ratio, the atmosphere is investigated. We do not detect clearly significant variations in the planet-to-star size ratio as function of wavelength. Although the ratio at the shortest measured wavelength, in g-band, is 2sigma larger than in the other bands. The uncertainties in the Ks and Kc bands are large, due to systematic features in the light curves. The tentative increase in the planet-to-star size ratio at the shortest wavelength could be a sign of an increase in the effective planet-size due to Rayleigh scattering, which would require GJ1214b to have a hydrogen-rich atmosphere. If true, then the atmosphere has to have both clouds, to suppress planet-size variations at red optical wavelengths, as well as a sub-solar metallicity, to suppress strong molecular features in the near- and mid-infrared However, star spots, which are known to be present on the hoststar's surface, can (partly) cancel out the expected variations in planet-to-star size ratio, because the lower surface temperature of the spots causes the effective size of the star to vary with wavelength. A hypothetical spot-fraction of 10%, corresponding to an average stellar dimming of 5% in the i-band, would be able to raise the near- and mid-infrared points sufficiently with respect to the optical measurements to be inconsistent with a water-dominated atmosphere. Modulation of the spot fraction due to the stellar rotation would in such case cause the observed flux variations of GJ1214.2012A&A...538A..46Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/538/A46CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/538/A46https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/538/A46http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/538/A46https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/538/A46https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/538/A46http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/538/A46GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/A+A/538/A46/transitsObservations of the transits of GJ 1214brecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJulian Date of observationdtime.epochdoubleFluxCorrected fluxphot.flux;arith.ratiofloate_FluxUncertainty on Fluxstat.error;phot.fluxfloatBand[girzI Kc Ks] Band of the fluxinstr.bandpasscharTelSimbad column added by the CDSmeta.id;instr.telchar