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Pollacco, D.; Skillen, I.; Collier Cameron, A.; Loeillet, B.; Stempels, H. C.; Bouchy, F.; Gibson, N. P.; Hebb, L.; Hebrard, G.; Joshi, Y. C.; McDonald, I.; Smalley, B.; Smith, A. M. S.; Street, R. A.; Udry, S.; West, R. G.; Wilson, D. M.; Wheatley, P. J.; Aigrain, S.; Alsubai, K.; Benn, C. R.; Bruce, V. A.; Christian, D. J.; Clarkson, W. I.; Enoch, B.; Evans, A.; Fitzsimmons, A.; Haswell, C. A.; Hellier, C.; Hickey, S.; Hodgkin, S. T.; Horne, K.; Hrudkova, M.; Irwin, J.; Kane, S. R.; Keenan, F. P.; Lister, T. A.; Maxted, P.; Mayor, M.; Moutou, C.; Norton, A. J.; Osborne, J. P.; Parley, N.; Pont, F.; Queloz, D.; Ryans, R. and Simpson, E.
(2008).
DOI: https://doi.org/10.1111/j.1365-2966.2008.12939.x
Abstract
We report the discovery of WASP-3b, the third transiting exoplanet to be discovered by the WASP and SOPHIE collaboration. WASP-3b transits its host star USNO-B1.0 1256?0285133 every 1.846 834 ± 0.000 002 d. Our high-precision radial velocity measurements present a variation with amplitude characteristic of a planetary-mass companion and in phase with the light curve. Adaptive optics imaging shows no evidence for nearby stellar companions, and line-bisector analysis excludes faint, unresolved binarity and stellar activity as the cause of the radial velocity variations. We make a preliminary spectroscopic analysis of the host star and find it to have Teff = 6400 ± 100 K and log g = 4.25 ± 0.05 which suggests it is most likely an unevolved main-sequence star of spectral type F7-8V. Our simultaneous modelling of the transit photometry and reflex motion of the host leads us to derive a mass of 1.76+0.08 -0.14 MJ and radius 1.31+0.07-0.14 RJ for WASP-3b. The proximity and relative temperature of the host star suggests that WASP-3b is one of the hottest exoplanets known, and thus has the potential to place stringent constraints on exoplanet atmospheric models.
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