Certain studies were made of the lunar surface based on measurements at visible and far infrared wavelengths obtained from a scan over the full Moon. The large number of data points available made it possible to refine the albedo statistics over the disk previously described by Sytinskaya (1953). The simultaneous measurements at the two wavelengths provided a factor for converting full Moon photometric brightness to bolometric albedo. The disk-averaged value of this parameter is consistent with previous photometric measurements. The brightness temperature statistics over the disk led to a replacement of the traditional cos1/6 θ law of temperature variation over the full Moon by an expression which is linear in cosθ.