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Post Info TOPIC: WASP-24b


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Title: Thermal emission from WASP-24b at 3.6 and 4.5 µm 
Authors: A. M. S. Smith, D. R. Anderson, N. Madhusudhan, J. Southworth, A. Collier Cameron, J. Harrington, C. Hellier, P. F. L. Maxted, D. Pollacco, D. Queloz, B. Smalley, A. H. M . J. Triaud, P. J. Wheatley

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.

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