Photometry of Palomar 5. Panels (a) and (b) compare the CFHT and SDSS photometry in a 1 square-degree field centered on the globular cluster remnant. The irregular polygon superimposed on (a) encompasses the stellar populations observed within the central ﹩15^{\prime} ﹩. The error bars show the average color and magnitude uncertainties for stars in the color range ﹩0.2\lt {(g-r)}_{0}\lt 0.7﹩, and are shown only when either the color or magnitude uncertainty exceeds 0.01 mag. Clearly the CFHT photometry provides a significant improvement over the SDSS in this region. We combine the CFHT and KPNO photometry in panels (c) and (d).