WASP-1b and WASP-2b: two new transiting exoplanets detected with SuperWASP and SOPHIE
Cameron, A. Collier ; Bouchy, F. ; Hébrard, G. ; Maxted, P. ; Pollacco, D. ; Pont, F. ; Skillen, I. ; Smalley, B. ; Street, R. A. ; West, R. G. ; Wilson, D. M. ; Aigrain, S. ; Christian, D. J. ; Clarkson, W. I. ; Enoch, B. ; Evans, A. ; Fitzsimmons, A. ; Fleenor, M. ; Gillon, M. ; Haswell, C. A. ; Hebb, L. ; Hellier, C. ; Hodgkin, S. T. ; Horne, K. ; Irwin, J. ; Kane, S. R. ; Keenan, F. P. ; Loeillet, B. ; Lister, T. A. ; Mayor, M. ; Moutou, C. ; Norton, A. J. ; Osborne, J. ; Parley, N. ; Queloz, D. ; Ryans, R. ; Triaud, A. H. M. J. ; Udry, S. ; Wheatley, P. J.
In: Monthly Notices of the Royal Astronomical Society, 2007, vol. 375, no. 3, p. 951-957
Zum persönliche Liste hinzufügen- Summary
- 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 radial-velocity 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