Triton's Surface Composition: Reevaluation of Voyager colors from the perspective of New Horizons at Pluto

New Horizons mapping of Pluto the best known Kuiper Belt Object (KBO), revealed the presence of surface ices (including CO, CH4, N2, and H2O) and their geologic distribution. Triton, the largest moon of Neptune, is very similar in size and bulk density to Pluto and was likely a KBO before capture. Both bodies orbit at comparable distances from the Sun (though Pluto goes further out) and have similar rotation periods. Both have complex obliquity cycles and both may have been or are ocean worlds. Triton is also a priority target for future exploration. Voyager (VGR) color mapping lacked the infrared capabilities of New Horizons (NH), rendering compositional mapping very difficult, but also revealed complex geologic and atmospheric color patterns on the surface of Triton. These include color changes at unit boundaries and equatorial bright and dark regional patterns uncorrelated to geology with very strong UV signatures. Small dark spots that appear wind-blown also have distinct spectral signatures. We have remapped the color data for Triton using updated cartography. VGR did extend into the UV which allows comparisons to Cassini icy moons color mapping. Color filter bandpasses for VGR & NH overlap in the 0.4 and 0.6 micron bands, which allows for a comparison of the brightness and spectral slopes of color units on the two bodies. The presence of CO2 on Triton will produce a distinct spectral signature compared to Pluto. Principle component analysis will be updated using all 6 filters to identify distinctive surface components. Disk integrated color rotational coverage from Earth-based spectra may also permit correlation of specific color units with identified longitudinal concentrations of ice phases.