Volume 563, March 2014
|Number of page(s)||13|
|Section||Planets and planetary systems|
|Published online||25 March 2014|
Transiting planets from WASP-South, Euler, and TRAPPIST
Institut d’Astrophysique et Géophysique, Université de Liège,
allée du 6 Août 17,
2 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK
3 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK
4 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
5 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
6 Cavendish Laboratory, Department of Physics, University of Cambridge, JJ Thomson Avenue, Cambridge, CB3 0HE, UK
7 N. Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland
8 Department of Physics and Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge MA 02139, USA
Accepted: 18 January 2014
Using the WASP transit survey, we report the discovery of three new hot Jupiters, WASP-68 b, WASP-73 b and WASP-88 b. The planet WASP-68 bhas a mass of 0.95 ± 0.03 MJup, a radius of 1.24-0.06+0.10 RJup, and orbits a V = 10.7 G0-type star (1.24 ± 0.03 M⊙ 1.69-0.06+0.11 R⊙, Teff = 5911 ± 60 K) with a period of 5.084298 ± 0.000015 days. Its size is typical of hot Jupiters with similar masses. The planet WASP-73 bis significantly more massive (1.88-0.06+0.07 MJup) and slightly larger (1.16-0.08+0.12 RJup) than Jupiter. It orbits a V = 10.5 F9-type star (1.34-0.04+0.05 M⊙, 2.07-0.08+0.19 R⊙, Teff = 6036 ± 120 K) every 4.08722 ± 0.00022 days. Despite its high irradiation (~2.3 × 109 erg s-1 cm-2), WASP-73 b has a high mean density (1.20-0.30+0.26 ρJup) that suggests an enrichment of the planet in heavy elements. The planet WASP-88 bis a 0.56 ± 0.08 MJuphot Jupiter orbiting a V = 11.4 F6-type star (1.45 ± 0.05 M⊙, 2.08-0.06+0.12 R⊙, Teff = 6431 ± 130 K) with a period of 4.954000 ± 0.000019 days. With a radius of 1.70-0.07+0.13 RJup, it joins the handful of planets with super-inflated radii. The ranges of ages we determine through stellar evolution modeling are 4.5–7.0 Gyr for WASP-68, 2.8-5.7 Gyr for WASP-73 and 1.8–4.3 Gyr for WASP-88. The star WASP-73 appears to be significantly evolved, close to or already in the subgiant phase. The stars WASP-68 and WASP-88 are less evolved, although in an advanced stage of core H-burning.
Key words: planetary systems / techniques: photometric / techniques: radial velocities / techniques: spectroscopic
Tables 1–3 are available in electronic form at http://www.aanda.org
The photometric time-series used in this work are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/563/A143
Chargée de recherches, Fonds de la Recherche Scientifique, FNRS, rue d’Egmont 5, 1000 Bruxelles, Belgium.
© ESO, 2014
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