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, Khalid Al-Subai, 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

Research output: Contribution to journalArticle

9 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 0.63 6-0.024 + 0.025 MJ and radius 1.653+0.090 -0.083 1.65 3-0.083 + 0.090 RJ. 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 e = 0.06 7-0.025 + 0.033) 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 0.57 1-0.035 + 0.034 MJ and 0.672 +0.049 -0.046 0.67 2-0.046 + 0.049 MJ, respectively; and radii of 1.092+0.035 -0.033 1.09 2-0.033 + 0.035 RJ for WASP-56b and 0.916+0.017 -0.014 0.91 6-0.014 + 0.017 RJ 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.

Original languageEnglish
Article numberA73
JournalAstronomy and Astrophysics
Volume551
DOIs
Publication statusPublished - 28 Feb 2013

Fingerprint

Jupiter (planet)
Jupiter
planets
planet
eccentric orbits
extrasolar planets
radii
orbits
main sequence stars
eclipses
heavy elements
thermal structure
eccentricity
brightness
physical property
physical properties
anomalies
anomaly
stars
orbitals

Keywords

  • Stars: individual: WASP-54
  • Stars: individual: WASP-56
  • Stars: individual: WASP-57
  • Techniques: photometric
  • Techniques: radial velocities

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Faedi, F., Pollacco, D., Barros, S. C. C., Brown, D., Collier Cameron, A., Doyle, A. P., ... 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

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.; Al-Subai, Khalid; 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.

In: Astronomy and Astrophysics, Vol. 551, A73, 28.02.2013.

Research output: Contribution to journalArticle

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, Al-Subai, K, 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, A73. https://doi.org/10.1051/0004-6361/201220520
Faedi F, Pollacco D, Barros SCC, Brown D, Collier Cameron A, Doyle AP et al. WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP. Astronomy and Astrophysics. 2013 Feb 28;551. A73. https://doi.org/10.1051/0004-6361/201220520
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. ; Al-Subai, Khalid ; 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. / WASP-54b, WASP-56b, and WASP-57b : Three new sub-Jupiter mass planets from SuperWASP. In: Astronomy and Astrophysics. 2013 ; Vol. 551.
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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 -0.024 0.63 6-0.024 + 0.025 MJ and radius 1.653+0.090 -0.083 1.65 3-0.083 + 0.090 RJ. 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 e = 0.06 7-0.025 + 0.033) 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 0.57 1-0.035 + 0.034 MJ and 0.672 +0.049 -0.046 0.67 2-0.046 + 0.049 MJ, respectively; and radii of 1.092+0.035 -0.033 1.09 2-0.033 + 0.035 RJ for WASP-56b and 0.916+0.017 -0.014 0.91 6-0.014 + 0.017 RJ 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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TY - JOUR

T1 - WASP-54b, WASP-56b, and WASP-57b

T2 - 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 - Al-Subai, Khalid

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 - 2013/2/28

Y1 - 2013/2/28

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 0.63 6-0.024 + 0.025 MJ and radius 1.653+0.090 -0.083 1.65 3-0.083 + 0.090 RJ. 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 e = 0.06 7-0.025 + 0.033) 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 0.57 1-0.035 + 0.034 MJ and 0.672 +0.049 -0.046 0.67 2-0.046 + 0.049 MJ, respectively; and radii of 1.092+0.035 -0.033 1.09 2-0.033 + 0.035 RJ for WASP-56b and 0.916+0.017 -0.014 0.91 6-0.014 + 0.017 RJ 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.

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 0.63 6-0.024 + 0.025 MJ and radius 1.653+0.090 -0.083 1.65 3-0.083 + 0.090 RJ. 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 e = 0.06 7-0.025 + 0.033) 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 0.57 1-0.035 + 0.034 MJ and 0.672 +0.049 -0.046 0.67 2-0.046 + 0.049 MJ, respectively; and radii of 1.092+0.035 -0.033 1.09 2-0.033 + 0.035 RJ for WASP-56b and 0.916+0.017 -0.014 0.91 6-0.014 + 0.017 RJ 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.

KW - Stars: individual: WASP-54

KW - Stars: individual: WASP-56

KW - Stars: individual: WASP-57

KW - Techniques: photometric

KW - Techniques: radial velocities

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