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WASP-54b, WASP-56b, and WASP-57b: three new sub-Jupiter mass planets from SuperWASP

Faedi, F.; Pollacco, D.; Barros, S. C. C.; Brown, D.; Collier Cameron, A.; Doyle, A. P.; Enoch, R.; Gillon, M.; Gómez Maqueo Chew, Y.; Hébrard, G.; Lendl, M.; Liebig, C.; Smalley, B.; Triaud, A. H. M. J.; West, R. G.; Wheatley, P. J.; Alsubai, K. A.; Anderson, D. R.; Armstrong, D.; Bento, J.; Bochinski, J.; Bouchy, F.; Busuttil, R.; Fossati, L.; Fumel, A.; Haswell, C.A.; Hellier, C.; Holmes, S.; Jehin, E.; Kolb, U.; McCormac, J.; Miller, G. R. M.; Moutou, C.; Norton, A. J.; Parley, N.; Queloz, D.; Santerne, A.; Skillen, I.; Smith, A. M. S.; Udry, S. and Watson, C. (2013). WASP-54b, WASP-56b, and WASP-57b: three new sub-Jupiter mass planets from SuperWASP. Astronomy & Astrophysics, 551 A73.

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DOI (Digital Object Identifier) Link: https://doi.org/10.1051/0004-6361/201220520
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Abstract

We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636+0.025-0.024MJ and radius 1.653+0.090-0.083RJ. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067+0.033-0.025) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V = 10.42 mag, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571+0.034-0.035MJ and 0.672+0.049-0.046MJ, respectively; and radii of 1.092+0.035-0.033RJ for WASP-56b and 0.916+0.017-0.014RJ for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as ~50 M⊕ in the case of WASP-57b. However,the composition of the deep interior of exoplanets remains still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets’ physical properties.

Item Type: Journal Item
Copyright Holders: 2012 ESO
ISSN: 1432-0746
Project Funding Details:
Funded Project NameProject IDFunding Body
OPTICONRG226604European Commission
Keywords: photometric techniques; radial velocities
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
Item ID: 36690
Depositing User: Andrew Norton
Date Deposited: 26 Feb 2013 11:02
Last Modified: 08 May 2019 15:16
URI: http://oro.open.ac.uk/id/eprint/36690
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