In order to attempt to observe a transit of a known exoplanet, one needs to know precisely where and when to look. The limiting factor for successfully observing a known exoplanet host star during the predicted transit time is often the precision of the transit ephemeris. Particularly for intermediate-long period planets, this predicted time is often only roughly known. The quality of a calculated transit ephemeris is primarily determined by (a) the uncertainties associated with the fitted orbital parameters, and (b) the time elapsed since the most recent radial velocity data was acquired. Acquiring new high precision radial velocity data can easily mitigate both effects. With a prompt photometric observing strategy after the orbital parameters have been revised, one can maximize the chances of being able to obtain complete coverage of the transit observing window and thus either confirm or rule out the transiting nature of the planet.