• DOI:10.1111/j.1365-2966.2006.11350.x
• Corpus ID: 735515

WASP-1b and WASP-2b: Two new transiting exoplanets detected with SuperWASP and SOPHIE

@article{Cameron2006WASP1bAW,
  title={WASP-1b and WASP-2b: Two new transiting exoplanets detected with SuperWASP and SOPHIE},
  author={Andrew Collier Cameron and François Bouchy and Guillaume H{\'e}brard and P. F. L. Maxted and Don Pollacco and Fr'ed'eric Pont and Ian Skillen and Barry Smalley and Rachel A. Street and Richard G. West and D. Mark Wilson and Suzanne Aigrain and Damian J. Christian and William I. Clarkson and B E Enoch and Aneurin Evans and Alan Fitzsimmons and Matthew Fleenor and Micha{\"e}l Gillon and Carole A. Haswell and Leslie Hebb and Coel Hellier and Simon T. Hodgkin and Keith D. Horne and Jonathan M. Irwin and Stephen R. Kane and Francis P. Keenan and B. Loeillet and Tim A. Lister and Michel Mayor and Claire Moutou and Andrew J. Norton and Julian P. Osborne and Neil R. Parley and Didier Queloz and Robert S. I. Ryans and Amaury H. M. J. Triaud and St{\'e}phane Udry and Peter J. Wheatley},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2006},
  volume={375},
  pages={951-957}
}

• A. Cameron, F. Bouchy, +36 authors P. Wheatley
• Published 25 September 2006
• Geology, Physics
• Monthly Notices of the Royal Astronomical Society

We have detected low-amplitude radial-velocity variations in two stars, USNO-B1.0 1219‐ 0005465 (GSC 02265‐00107 = WASP‐1) and USNO-B1.0 0964‐0543604 (GSC 00522‐ 01199 = WASP‐2). Both stars were identified as being likely host stars of transiting exoplanets in the 2004 SuperWASP wide-field transit survey. Using the newly commissioned radial-velocity spectrograph SOPHIE at the Observatoire de Haute-Provence, we found that both objects exhibit reflex orbital radial-velocity variations with amplitudes characteristic of planetary-mass companions and in-phase with the photometric orbits. Line-bisector studies rule out faint blended binaries as the cause of either the radial-velocity variations or the transits. We perform preliminary spectral analyses of the host stars, which together with their radialvelocity variations and fits to the transit light curves yield estimates of the planetary masses and radii. WASP-1b and WASP-2b have orbital periods of 2.52 and 2.15 d, respectively. Given mass estimates for their F7V and K1V primaries, we derive planet masses 0.80‐0.98 and 0.81‐ 0.95 times that of Jupiter, respectively. WASP-1b appears to have an inflated radius of at least 1.33 RJup, whereas WASP-2b has a radius in the range 0.65‐1.26 RJup.