  Transit (TR) surveys for extrasolar planets have recently uncovered a
population of ``very hot Jupiters,'' planets with orbital periods of P< 3 d. At
first sight this may seem surprising, given that radial velocity (RV) surveys
have found a dearth of such planets, despite the fact that their sensitivity
increases with decreasing P. We examine the confrontation between RV and TR
survey results, paying particular attention to selection biases that favor
short-period planets in transit surveys. We demonstrate that, when such biases
and small-number statistics are properly taken into account, the period
distribution of planets found by RV and TR surveys are consistent at better
than the 1-sigma level. This consistency holds for a large range of reasonable
assumptions. In other words, there are not enough planets detected to robustly
conclude that the RV and TR short-period planet results are inconsistent.
Assuming a logarithmic distribution of periods, we find that the relative
frequency of very hot Jupiters (VHJ: P=1-3 d) to hot Jupiters (HJ: P=3-9 d) is
10-20%. Given an absolute frequency of HJ of ~1%, this implies that
approximately one star in ~500-1000 has a VHJ. We also note that VHJ and HJ
appear to be distinct in terms of their upper mass limit. We discuss the
implications of our results for planetary migration theories, as well as
present and future TR and RV surveys.
