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dc.contributor.authorNikolov, N.
dc.contributor.authorSing, David K.
dc.contributor.authorBurrows, A.S.
dc.contributor.authorFortney, J.J.
dc.contributor.authorHenry, G.
dc.contributor.authorPont, F.
dc.contributor.authorBallester, G.
dc.contributor.authorAigrain, Suzanne
dc.contributor.authorWilson, Paul A.
dc.contributor.authorHuitson, Catherine M.
dc.contributor.authorGibson, N.
dc.contributor.authorDesert, J.-M.
dc.contributor.authorLecavelier des Etangs, A.
dc.contributor.authorShowman, A.P.
dc.contributor.authorVidal-Madjar, A.
dc.contributor.authorWakeford, H.R.
dc.contributor.authorZahnle, K.
dc.date.accessioned2014-12-19T13:23:31Z
dc.date.issued2014
dc.description.abstractWe report Hubble Space Telescope optical to near-infrared transmission spectroscopy of the hot-Jupiter WASP-6b, measured with the Space Telescope Imaging Spectrograph and Spitzer's InfraRed Array Camera. The resulting spectrum covers the range 0.29–4.5 μm. We find evidence for modest stellar activity of WASP-6 and take it into account in the transmission spectrum. The overall main characteristic of the spectrum is an increasing radius as a function of decreasing wavelength corresponding to a change of Δ (Rp / R*) = 0.0071 from 0.33 to 4.5 μm. The spectrum suggests an effective extinction cross-section with a power law of index consistent with Rayleigh scattering, with temperatures of 973 ± 144 K at the planetary terminator. We compare the transmission spectrum with hot-Jupiter atmospheric models including condensate-free and aerosol-dominated models incorporating Mie theory. While none of the clear-atmosphere models is found to be in good agreement with the data, we find that the complete spectrum can be described by models that include significant opacity from aerosols including Fe-poor Mg2SiO4, MgSiO3, KCl and Na2S dust condensates. WASP-6b is the second planet after HD 189733b which has equilibrium temperatures near ∼1200 K and shows prominent atmospheric scattering in the optical.en_GB
dc.description.sponsorshipEuropean Research Council under the European Union's Seventh Framework Programmeen_GB
dc.description.sponsorshipERC(European Research Council)en_GB
dc.description.sponsorshipSTFC (Science & Technology Facilities Council)en_GB
dc.description.sponsorshipSpace Telescope Science Instituteen_GB
dc.identifier.citationVol. 447 (1), pp. 463 - 478en_GB
dc.identifier.doi10.1093/mnras/stu2433
dc.identifier.grantnumberFP7/2007-2013en_GB
dc.identifier.grantnumber336792en_GB
dc.identifier.grantnumberST/J0016/1en_GB
dc.identifier.grantnumberHST-GO-12473en_GB
dc.identifier.urihttp://hdl.handle.net/10871/16091
dc.language.isoenen_GB
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_GB
dc.relation.urlhttp://dx.doi.org/10.1093/mnras/stu2433en_GB
dc.subjectmethods: observationalen_GB
dc.subjecttechniques: spectroscopicen_GB
dc.subjectplanets and satellites: atmospheresen_GB
dc.subjectstars: activityen_GB
dc.subjectplanets and satellites: individual: WASP-6ben_GB
dc.titleHST hot-Jupiter transmission spectral survey: Haze in the atmosphere of WASP-6ben_GB
dc.typeArticleen_GB
dc.date.available2014-12-19T13:23:31Z
dc.identifier.issn0035-8711
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_GB
dc.identifier.eissn1365-2966
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen_GB


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