  We derive the frequencies of hot Jupiters (HJs) with 3--5 day periods and
very hot Jupiters (VHJs) with 1-3 day periods by comparing the planets actually
detected in the OGLE-III survey with those predicted by our models. The models
are constructed following Gould & Morgan (2003) by populating the line of sight
with stars drawn from the Hipparcos catalog. Using these, we demonstrate that
the number of stars with sensitivity to HJs and VHJs is only 4--16% of those in
the OGLE-III fields satisfying the spectroscopic-followup limit of V_max<17.5.
Hence, the frequencies we derive are much higher than a naive estimate would
indicate. We find that at 90% confidence the fraction of stars with planets in
the two period ranges is (1/310)(1^{+1.39}_{-0.59}) for HJs and
(1/690)(1^{+1.10}_{-0.54}) for VHJs. The HJ rate is statistically
indistinguishable from that found in radial velocity (RV) studies. However, we
note that magnitude-limited RV samples are heavily biased toward metal-rich
(hence, planet-bearing) stars, while transit surveys are not, and therefore we
expect that more sensitive transit surveys should find a deficit of HJs as
compared to RV surveys. The detection of 3 transiting VHJs, all with periods
less than 2 days, is marginally consistent with the complete absence of such
detections in RV surveys. The planets detected are consistent with being
uniformly distributed between 1.00 and 1.25 Jovian radii, but there are too few
in the sample to map this distribution in detail.
