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Thermal emission from WASP-24b at 3.6 and 4.5 μm
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dc.contributor.author | Smith, Alexis Michael Sheridan | |
dc.contributor.author | Anderson, D. R. | |
dc.contributor.author | Madhusudhan, N. | |
dc.contributor.author | Southworth, J. | |
dc.contributor.author | Cameron, Andrew Collier | |
dc.contributor.author | Blecic, J. | |
dc.contributor.author | Harrington, J. | |
dc.contributor.author | Hellier, C. | |
dc.contributor.author | Maxted, P. F. L. | |
dc.contributor.author | Pollacco, D. | |
dc.contributor.author | Queloz, D. | |
dc.contributor.author | Smalley, B. | |
dc.contributor.author | Triaud, A. H. M. J. | |
dc.contributor.author | Wheatley, P. J. | |
dc.date.accessioned | 2016-02-05T12:40:13Z | |
dc.date.available | 2016-02-05T12:40:13Z | |
dc.date.issued | 2012-09-01 | |
dc.identifier.citation | Smith , A M S , Anderson , D R , Madhusudhan , N , Southworth , J , Cameron , A C , Blecic , J , Harrington , J , Hellier , C , Maxted , P F L , Pollacco , D , Queloz , D , Smalley , B , Triaud , A H M J & Wheatley , P J 2012 , ' Thermal emission from WASP-24b at 3.6 and 4.5 μm ' , Astronomy & Astrophysics , vol. 545 . https://doi.org/10.1051/0004-6361/201219294 | en |
dc.identifier.issn | 0004-6361 | |
dc.identifier.other | PURE: 240468044 | |
dc.identifier.other | PURE UUID: c773ca73-37e9-4e29-916b-3bdef77456ad | |
dc.identifier.other | BibCode: 2012A&A...545A..93S | |
dc.identifier.other | Scopus: 84866279157 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/58531421 | |
dc.identifier.uri | http://hdl.handle.net/10023/8144 | |
dc.description.abstract | Aims. We observe occultations of WASP-24b to measure brightness temperatures and to determine whether or not its atmosphere exhibits a thermal inversion (stratosphere). Methods. We observed occultations of WASP-24b at 3.6 and 4.5 μm using the Spitzer Space Telescope. It has been suggested that there is a correlation between stellar activity and the presence of inversions, so we analysed existing HARPS spectra in order to calculate log R′HK for WASP-24 and thus determine whether or not the star is chromospherically active. We also observed a transit of WASP-24b in the Strömgren u and y bands, with the CAHA 2.2-m telescope. Results. We measure occultation depths of 0.159 ± 0.013 per cent at 3.6 μm and 0.202 ± 0.018 per cent at 4.5 μm. The corresponding planetary brightness temperatures are 1974 ± 71 K and 1944 ± 85 K respectively. Atmosphere models with and without a thermal inversion fit the data equally well; we are unable to constrain the presence of an inversion without additional occultation measurements in the near-IR. We find log R′HK = −4.98 ± 0.12, indicating that WASP-24 is not a chromospherically active star. Our global analysis of new and previously-published data has refined the system parameters, and we find no evidence that the orbit of WASP-24b is non-circular. Conclusions. These results emphasise the importance of complementing Spitzer measurements with observations at shorter wavelengths to gain a full understanding of hot Jupiter atmospheres. | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomy & Astrophysics | en |
dc.rights | Copyright ESO 2012. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1051/0004-6361/201219294. | en |
dc.subject | Planetary systems | en |
dc.subject | Planets and satellites: atmospheres | en |
dc.subject | Stars: individual: WASP-24 | en |
dc.subject | Planets and satellites: individual: WASP-24b | en |
dc.subject | Infrared: planetary systems | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Thermal emission from WASP-24b at 3.6 and 4.5 μm | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.description.version | Publisher PDF | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1051/0004-6361/201219294 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | http://adsabs.harvard.edu/abs/2012A%26A...545A..93S | en |
dc.identifier.grantnumber | ST/J001651/1 | en |
dc.identifier.grantnumber | PP/F000065/1 | en |
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