  Of the known transiting extra-solar planets, a few have been detected through
photometric follow-up observations of radial velocity planets. Perhaps the best
known of these is the transiting exoplanet HD 209458b. For hot Jupiters
(periods less than ~5 days), the a priori information that 10% of these planets
will transit their parent star due to the geometric transit probability leads
to an estimate of the expected transit yields from radial velocity surveys. The
radial velocity information can be used to construct an effective photometric
follow-up strategy which will provide optimal detection of possible transits.
Since the planet-harbouring stars are already known in this case, one is only
limited by the photometric precision achieveable by the chosen
telescope/instrument. The radial velocity modelling code presented here
automatically produces a transit ephemeris for each planet dataset fitted by
the program. Since the transit duration is brief compared with the fitted
period, we calculate the maximum window for obtaining photometric transit
observations after the radial velocity data have been obtained, generalising
for eccentric orbits. We discuss a typically employed survey strategy which may
contribute to a possible radial velocity bias against detection of the very hot
Jupiters which have dominated the transit discoveries. Finally, we describe how
these methods can be applied to current and future radial velocity surveys.
