We propose to study of flows in the solar photosphere and their relationship to the distribution of magnetic flux. Our primary goals are threefold: 1) to obtain the spectrum, structure and evolution of convection as manifested in the photosphere, 2) to track the emergence and distribution of flux over the solar surface, and 3) to understand the interrelations between the fields and flows in the photosphere. To this end we need sequences of continuum, line-intensity and equivalent widths images with a cadence of 60 seconds and magnetograms no further apart than three hours.