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dc.contributor.authorKreidberg, Laura
dc.contributor.authorLine, Michael R.
dc.contributor.authorParmentier, Vivien
dc.contributor.authorStevenson, K. B.
dc.contributor.authorLouden, Tom
dc.contributor.authorBonnefoy, Mickäel
dc.contributor.authorFaherty, Jacqueline K.
dc.contributor.authorHenry, G.
dc.contributor.authorWilliamson, Michael H.
dc.contributor.authorStassun, Keivan
dc.contributor.authorBeatty, Thomas G.
dc.contributor.authorBean, Jacob L.
dc.contributor.authorFortney, Jonathan J.
dc.contributor.authorShowman, Adam P.
dc.contributor.authorDesert, Jean-Michel
dc.contributor.authorArcangeli, Jacob
dc.date.accessioned2018-08-15T17:20:43Z
dc.date.available2018-08-15T17:20:43Z
dc.date.issued2018-07
dc.identifier.citationLaura Kreidberg et al 2018 AJ 156 17en_US
dc.identifier.issn1538-3881
dc.identifier.doi10.3847/1538-3881/aac3df
dc.identifier.urihttp://hdl.handle.net/10150/628532
dc.description.abstractWe present thermal phase curve measurements for the hot Jupiter WASP-103b observed with Hubble/WFC3 and Spitzer IIRAC. The phase curves have large amplitudes and negligible hotspot offsets, indicative of poor heat redistribution to the nightside. We fit the phase variation with a range of climate maps and find that a spherical harmonics model generally provides the best fit. The phase-resolved spectra are consistent with blackbodies in the WFC3 bandpass, with brightness temperatures ranging from 1880 +/- 40 K on the nightside to 2930 +/- 40 K on the dayside. The dayside spectrum has a significantly higher brightness temperature in the Spitzer bands, likely due to CO emission and a thermal inversion. The inversion is not present on the nightside. We retrieved the atmospheric composition and found that it is moderately metal-enriched ([M/H] = 23(-13)(+29) x solar) and the carbon-to-oxygen ratio is below 0.9 at 3 sigma confidence. In contrast to cooler hot Jupiters, we do not detect spectral features from water, which we attribute to partial H2O dissociation. We compare the phase curves to 3D general circulation models and find that magnetic drag effects are needed to match the data. We also compare the WASP-103b spectra to brown dwarfs and young, directly imaged companions. We find that these objects have significantly larger water features, indicating that surface gravity and irradiation environment play an important role in shaping the spectra of hot Jupiters. These results highlight the 3D structure of exoplanet atmospheres and illustrate the importance of phase curve observations for understanding their complex chemistry and physics.en_US
dc.description.sponsorshipNASA through Space Telescope Science Institute [GO-15050]; NASA [NAS 5-2655511099]; NASA through JPL/Caltech [11099]; National Aeronautics and Space Administration; David and Lucile Packard Foundation; European Research Council (ERC) [679633]; Tennessee State University; NASA XRP [NNX17AB56G]; State of Tennessee through its Centers of Excellence Programen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/1538-3881/156/i=1/a=17?key=crossref.4f1f117aaf5c91f847ec2fabdedbc13cen_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectplanets and satellites: atmospheresen_US
dc.subjectplanets and satellites: gaseous planetsen_US
dc.subjectplanets and satellites: individual (WASP-103b)en_US
dc.titleGlobal Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b from HST and Spitzer Phase Curve Observationsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Planetary Scien_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalASTRONOMICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astronomical Journal
dc.source.volume156
dc.source.issue1
dc.source.beginpage17
refterms.dateFOA2018-08-15T17:20:43Z


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