WASP-3b: a strongly irradiated transiting gas-giant planet

D. Pollacco, I. Skillen, A. Collier Cameron, B. Loeillet, H.~C. Stempels, F. Bouchy, N.~P. Gibson, L. Hebb, G. Hébrard, Y.~C. Joshi, I. McDonald, B. Smalley, A.~M.~S. Smith, R.~A. Street, S. Udry, R.~G. West, D.~M. Wilson, P.~J. Wheatley, S. Aigrain, K. AlsubaiC.~R. Benn, V.~A. Bruce, D.~J. Christian, W.~I. Clarkson, B. Enoch, A. Evans, A. Fitzsimmons, C.~A. Haswell, C. Hellier, S. Hickey, S.~T. Hodgkin, K. Horne, M. Hrudková, J. Irwin, S.~R. Kane, F.~P. Keenan, T.~A. Lister, P. Maxted, M. Mayor, C. Moutou, A.~J. Norton, J.~P. Osborne, N. Parley, F. Pont, D. Queloz, R. Ryans, E. Simpson

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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-B1.01256-0285133 every 1.846834 +/- 0.000002 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 +/- 100K 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.
Original languageEnglish
Pages (from-to)1576-1584
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Publication statusPublished - 11 Apr 2008

ASJC Scopus subject areas

  • Space and Planetary Science


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