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

F. Faedi; D. Pollacco; S.~C.~C. Barros; D. Brown; A. Collier Cameron; A.~P. Doyle; R. Enoch; M. Gillon; Y. Gómez Maqueo Chew; G. Hébrard; M. Lendl; C. Liebig; B. Smalley; A.~H.~M.~J. Triaud; R.~G. West; P.~J. Wheatley; K.~A. Alsubai; D.~R. Anderson; D. Armstrong; J. Bento; J. Bochinski; F. Bouchy; R. Busuttil; L. Fossati; A. Fumel; C.~A. Haswell; C. Hellier; S. Holmes; E. Jehin; U. Kolb; J. McCormac; G.~R.~M. Miller; C. Moutou; A.~J. Norton; N. Parley; D. Queloz; A. Santerne; I. Skillen; A.~M.~S. Smith; S. Udry; C. Watson

doi:10.1051/0004-6361/201220520

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

F. Faedi, D. Pollacco, S.~C.~C. Barros, D. Brown, A. Collier Cameron, A.~P. Doyle, R. Enoch, M. Gillon, Y. Gómez Maqueo Chew, G. Hébrard, M. Lendl, C. Liebig, B. Smalley, A.~H.~M.~J. Triaud, R.~G. West, P.~J. Wheatley, K.~A. Alsubai, D.~R. Anderson, D. Armstrong, J. BentoJ. Bochinski, F. Bouchy, R. Busuttil, L. Fossati, A. Fumel, C.~A. Haswell, C. Hellier, S. Holmes, E. Jehin, U. Kolb, J. McCormac, G.~R.~M. Miller, C. Moutou, A.~J. Norton, N. Parley, D. Queloz, A. Santerne, I. Skillen, A.~M.~S. Smith, S. Udry, C. Watson

Physics and Astronomy

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12 Citations (Scopus)

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$$_-0.024$R$_J$. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067$^+0.033$$_-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$$_-0.035$M$_J$ and 0.672$^+0.049$$_-0.046$M$_J$, respectively; and radii of 1.092$^+0.035$$_-0.033$R$_J$ for WASP-56b and 0.916$^+0.017$$_-0.014$R$_J$ 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. RV data (Tables 6-9) are available in electronic form at http://www.aanda.orgPhotometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A73

Original language	English
Pages (from-to)	A73
Journal	Astronomy and Astrophysics
Volume	551
DOIs	https://doi.org/10.1051/0004-6361/201220520
Publication status	Published - 1 Mar 2013

Keywords

techniques: photometric, techniques: radial velocities, stars: individual: WASP-54, stars: individual: WASP-56, stars: individual: WASP-57

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10.1051/0004-6361/201220520

Cite this

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., ... Watson, C. (2013). WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP. Astronomy and Astrophysics, 551, A73. https://doi.org/10.1051/0004-6361/201220520

@article{f3d15095315a42f58afc7298d030c8f0,

title = "WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP",

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$$_-0.024$R$_J$. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067$^+0.033$$_-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$$_-0.035$M$_J$ and 0.672$^+0.049$$_-0.046$M$_J$, respectively; and radii of 1.092$^+0.035$$_-0.033$R$_J$ for WASP-56b and 0.916$^+0.017$$_-0.014$R$_J$ 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. RV data (Tables 6-9) are available in electronic form at http://www.aanda.orgPhotometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A73 ",

keywords = "techniques: photometric, techniques: radial velocities, stars: individual: WASP-54, stars: individual: WASP-56, stars: individual: WASP-57",

author = "F. Faedi and D. Pollacco and S.~C.~C. Barros and D. Brown and {Collier Cameron}, A. and A.~P. Doyle and R. Enoch and M. Gillon and {G{\'o}mez Maqueo Chew}, Y. and G. H{\'e}brard and M. Lendl and C. Liebig and B. Smalley and A.~H.~M.~J. Triaud and R.~G. West and P.~J. Wheatley and K.~A. Alsubai and D.~R. Anderson and D. Armstrong and J. Bento and J. Bochinski and F. Bouchy and R. Busuttil and L. Fossati and A. Fumel and C.~A. Haswell and C. Hellier and S. Holmes and E. Jehin and U. Kolb and J. McCormac and G.~R.~M. Miller and C. Moutou and A.~J. Norton and N. Parley and D. Queloz and A. Santerne and I. Skillen and A.~M.~S. Smith and S. Udry and C. Watson",

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month = mar,

day = "1",

doi = "10.1051/0004-6361/201220520",

language = "English",

volume = "551",

pages = "A73",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Faedi, F, Pollacco, D, Barros, SCC, Brown, D, Collier Cameron, A, Doyle, AP, Enoch, R, Gillon, M, Gómez Maqueo Chew, Y, Hébrard, G, Lendl, M, Liebig, C, Smalley, B, Triaud, AHMJ, West, RG, Wheatley, PJ, Alsubai, KA, Anderson, DR, Armstrong, D, Bento, J, Bochinski, J, Bouchy, F, Busuttil, R, Fossati, L, Fumel, A, Haswell, CA, Hellier, C, Holmes, S, Jehin, E, Kolb, U, McCormac, J, Miller, GRM, Moutou, C, Norton, AJ, Parley, N, Queloz, D, Santerne, A, Skillen, I, Smith, AMS, Udry, S & Watson, C 2013, 'WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP', Astronomy and Astrophysics, vol. 551, pp. A73. https://doi.org/10.1051/0004-6361/201220520

TY - JOUR

T1 - WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP

AU - Faedi, F.

AU - Pollacco, D.

AU - Barros, S.~C.~C.

AU - Brown, D.

AU - Collier Cameron, A.

AU - Doyle, A.~P.

AU - Enoch, R.

AU - Gillon, M.

AU - Gómez Maqueo Chew, Y.

AU - Hébrard, G.

AU - Lendl, M.

AU - Liebig, C.

AU - Smalley, B.

AU - Triaud, A.~H.~M.~J.

AU - West, R.~G.

AU - Wheatley, P.~J.

AU - Alsubai, K.~A.

AU - Anderson, D.~R.

AU - Armstrong, D.

AU - Bento, J.

AU - Bochinski, J.

AU - Bouchy, F.

AU - Busuttil, R.

AU - Fossati, L.

AU - Fumel, A.

AU - Haswell, C.~A.

AU - Hellier, C.

AU - Holmes, S.

AU - Jehin, E.

AU - Kolb, U.

AU - McCormac, J.

AU - Miller, G.~R.~M.

AU - Moutou, C.

AU - Norton, A.~J.

AU - Parley, N.

AU - Queloz, D.

AU - Santerne, A.

AU - Skillen, I.

AU - Smith, A.~M.~S.

AU - Udry, S.

AU - Watson, C.

PY - 2013/3/1

Y1 - 2013/3/1

N2 - 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$$_-0.024$R$_J$. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067$^+0.033$$_-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$$_-0.035$M$_J$ and 0.672$^+0.049$$_-0.046$M$_J$, respectively; and radii of 1.092$^+0.035$$_-0.033$R$_J$ for WASP-56b and 0.916$^+0.017$$_-0.014$R$_J$ 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. RV data (Tables 6-9) are available in electronic form at http://www.aanda.orgPhotometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A73

AB - 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$$_-0.024$R$_J$. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (e = 0.067$^+0.033$$_-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$$_-0.035$M$_J$ and 0.672$^+0.049$$_-0.046$M$_J$, respectively; and radii of 1.092$^+0.035$$_-0.033$R$_J$ for WASP-56b and 0.916$^+0.017$$_-0.014$R$_J$ 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. RV data (Tables 6-9) are available in electronic form at http://www.aanda.orgPhotometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A73

KW - techniques: photometric, techniques: radial velocities, stars: individual: WASP-54, stars: individual: WASP-56, stars: individual: WASP-57

U2 - 10.1051/0004-6361/201220520

DO - 10.1051/0004-6361/201220520

M3 - Article

SN - 0004-6361

VL - 551

SP - A73

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

ER -

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

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Keywords

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