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

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Cameron_2013_AA_WASP54b.pdf (1.903Mb)
Date
03/2013
Author
Faedi, F.
Pollacco, D.
Barros, S.C.C.
Brown, David John Alexander
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.
Watson, C.
Funder
Science & Technology Facilities Council
Science & Technology Facilities Council
Grant ID
ST/J001651/1
PP/F000065/1
Keywords
Techniques: photometric
Techniques: radial velocities
Stars: individual: WASP-54
Stars: individual: WASP-56
Stars: individual: WASP-57
QB Astronomy
QC Physics
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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.
Citation
Faedi , F , Pollacco , D , Barros , S C C , Brown , D J A , 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 & Watson , C 2013 , ' WASP-54b, WASP-56b, and WASP-57b : three new sub-Jupiter mass planets from SuperWASP ' , Astronomy & Astrophysics , vol. 551 , A73 . https://doi.org/10.1051/0004-6361/201220520
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201220520
ISSN
0004-6361
Type
Journal article
Rights
© ESO, 2013. Reproduced with permission from Astronomy & Astrophysics, © ESO
Collections
  • University of St Andrews Research
URL
http://www.aanda.org/articles/aa/full_html/2013/03/aa20520-12/aa20520-12.html#S16
URI
http://hdl.handle.net/10023/5478

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