The I‐band magnitude distribution for all identified radio galaxies. The fluxes of sources where only V‐band observations are available are converted assuming the SDSS DR5 colors described in § 3.2, Fig. 5, and Fig. 6. The vertical dashed line shows the flux‐averaged, 50% completeness depth of the fields, while the arrows represent the depths of the eight fields where no optical counterpart was identified to their respective field limits. This peak at ﹩I\simeq 20.7\pm 0.5﹩ mag is nearly 3 mag brighter than the depth of the typical WFPC2 field. The source counts of a random population of field galaxies should increase as a power‐law to the completeness limit of the field, contrary to what is seen for the radio‐selected galaxies.