We have computed the photometric magnitudes of rotating atmospheres-based on the simple model of Collins-for a grid suitable for main-sequence and slightly evolved stars of spectral type A0 to F5. A gravity-darkening law valid for radiative and convective envelopes has been considered. The general results are given as magnitude differences between rotating and non-rotating copartners to allow for the use of any photometric calibration. A simple interpolation on these results gives the photometric parameters for interior rotating models but we also indicate how they can be used to correct for the effect of rotation when an investigation with non-rotating models is carried out. We illustrate the procedure with the interesting case of the Praesepe Cluster.