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.

DOI: https://doi.org/10.1051/0004-6361/201220520

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.

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About

• Item ORO ID
• 36690
• Item Type
• Journal Item
• ISSN
• 1432-0746
• Project Funding Details

• Funded Project Name	Project ID	Funding Body
  OPTICON	RG226604	European Commission

• Keywords
• photometric techniques; radial velocities
• Academic Unit or School
• Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
  Faculty of Science, Technology, Engineering and Mathematics (STEM)
• Copyright Holders
• © 2012 ESO
• Depositing User
• Andrew Norton