Modeling of Triton's spectrum indicates a bright scattering layer of optical depth &tgr;≂3 overlying an optically deep layer of CH4 with high absorption and little scattering. UV absorption in the spectrum indicates &tgr;~0.3 of red-yellow haze, although some color may also arise from complex organics partially visible on the surface. An analysis of this and other (spectro)photometric evidence indicates that Triton most likely has a bright surface, which was partially visible in 1977--1980. Geometric albedo p=0.62+0.18-0.12, radius r=1480¿180 km, and temperature T=48¿6 K. With scattering optical depths of 0.3--3 and ~1--10 mb of N2, a Mars-like atmospheric density and surface visibility pertain. Imaging with the 0.62 &mgr;m CH4 filter of the Voyager 2 wide angle camera could show ~20% contrast between the average surface and clean exposures of CH4 ice (which is not limited to the polar caps). Low far-infrared atmospheric opacity will in principle allow the detection of thermal gradients in the surface caused by optically transmitting but infrared opaque CH4 and N2 ice. ¿ American Geophysical Union 1989