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There are a handful of spectral windows in the near-IR through which we cansee down to Venus' surface on the night side of the planet. The surface of oursister planet has thus been imaged by sensors on Venus-orbiting platforms(Venus Express, Akatsuki) and during fly-by with missions to other planets(Galileo, Cassini). The most tantalizing finding, so far, is the hint ofpossible active volcanism. However, the thermal radiation emitted by thesearing (c. 475 degrees C) surface of Venus has to get through the opaqueclouds between 50 and 70 km altitude, as well as the sub-cloud atmosphere. Inthe clouds, the light is not absorbed but scattered, many times. This resultsin blurring the surface imagery to the point where the smallest discerniblefeature is roughly 100 km in size, full-width half-max (FWHM), and this hasbeen explained using numerical models. We describe a new analytical modelingframework for predicting the width of the atmospheric point-spread function(APSF), which is what determines the effective resolution of surface imagingfrom space. Our best estimates of the APSF width for the 1-to-1.2 micronspectral range are clustered around 130 km FWHM. Interestingly, this issomewhat larger than the accepted value of about 100 km, which is based onvisual image inspection and numerical simulations.

Imaging Venus' Surface at Night in the Near-IR From Above Its Clouds: New Analytical Theory for the Effective Spatial Resolution