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Parker Solar Probe (PSP) conducted several flybys of Venus while using Venus'gravity for orbital adjustments to enable its daring passes of the Sun. Duringthese flybys, PSP turned to image the nightside of Venus using the Wide-fieldImager for Solar PRobe (WISPR) optical telescopes, which unexpectedly observedVenus' surface through its thick and cloudy atmosphere in a theorized, butuntil-then unobserved near-visible spectral window below 0.8 $\mu$m. We useobservations taken during PSP's fourth Venus gravity assist flyby to examinethe origin of the Venus nightside flux and confirm the presence of this newatmospheric window through which to observe the surface geology of Venus. TheWISPR images are well explained by emission from the hot Venus surface escapingthrough a new atmospheric window in the optical with an overlying emissioncomponent from the atmosphere at the limb that is consistent with O$_2$nightglow. The surface thermal emission correlates strongly with surfaceelevation (via temperature) and emission angle. Tessera and plains units havedistinct WISPR brightness values. Controlling for elevation, Ovda Regio tesserais brighter than Thetis Regio; likewise, the volcanic plains of SogolonPlanitia are brighter than the surrounding regional plains units. WISPRbrightness at 0.8 $\mu$m is predicted to be positively correlated to FeOcontent in minerals; thus, the brighter units may have a different startingcomposition, be less weathered, or have larger particle sizes.

A WISPR of the Venus Surface: Analysis of the Venus Nightside Thermal Emission at Optical Wavelengths