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dc.contributor.authorFaedi, F.
dc.contributor.authorPollacco, D.
dc.contributor.authorBarros, S.C.C.
dc.contributor.authorBrown, David John Alexander
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorDoyle, A.P.
dc.contributor.authorEnoch, R.
dc.contributor.authorGillon, M.
dc.contributor.authorGómez Maqueo Chew, Y.
dc.contributor.authorHébrard, G.
dc.contributor.authorLendl, M.
dc.contributor.authorLiebig, C.
dc.contributor.authorSmalley, B.
dc.contributor.authorTriaud, A.H.M.J.
dc.contributor.authorWest, R.G.
dc.contributor.authorWheatley, P.J.
dc.contributor.authorAlsubai, K.A.
dc.contributor.authorAnderson, D.R.
dc.contributor.authorArmstrong, D.
dc.contributor.authorBento, J.
dc.contributor.authorBochinski, J.
dc.contributor.authorBouchy, F.
dc.contributor.authorBusuttil, R.
dc.contributor.authorFossati, L.
dc.contributor.authorFumel, A.
dc.contributor.authorHaswell, C.A.
dc.contributor.authorHellier, C.
dc.contributor.authorHolmes, S.
dc.contributor.authorJehin, E.
dc.contributor.authorKolb, U.
dc.contributor.authorMcCormac, J.
dc.contributor.authorMiller, G.R.M.
dc.contributor.authorMoutou, C.
dc.contributor.authorNorton, A.J.
dc.contributor.authorParley, N.
dc.contributor.authorQueloz, D.
dc.contributor.authorSanterne, A.
dc.contributor.authorSkillen, I.
dc.contributor.authorSmith, A.M.S.
dc.contributor.authorUdry, S.
dc.contributor.authorWatson, C.
dc.date.accessioned2014-09-23T12:01:09Z
dc.date.available2014-09-23T12:01:09Z
dc.date.issued2013-03
dc.identifier.citationFaedi , 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/10.1051/0004-6361/201220520en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 150580589
dc.identifier.otherPURE UUID: 1d66f6b6-bcac-4fdd-b5d0-8b563d166204
dc.identifier.otherScopus: 84874250376
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531465
dc.identifier.urihttp://hdl.handle.net/10023/5478
dc.description.abstractWe 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.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2013. Reproduced with permission from Astronomy & Astrophysics, © ESOen
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectStars: individual: WASP-54en
dc.subjectStars: individual: WASP-56en
dc.subjectStars: individual: WASP-57en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleWASP-54b, WASP-56b, and WASP-57b : three new sub-Jupiter mass planets from SuperWASPen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201220520
dc.description.statusPeer revieweden
dc.identifier.urlhttp://www.aanda.org/articles/aa/full_html/2013/03/aa20520-12/aa20520-12.html#S16en


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