  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 days respectively. Given mass estimates for their F7V and K1V
primaries we derive planet masses 0.80 to 0.98 and 0.81 to 0.95 times that of
Jupiter respectively. WASP-1b appears to have an inflated radius of at least
1.33 R_Jup, whereas WASP-2b has a radius in the range 0.65 to 1.26 R_Jup.
