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Future space-based direct imaging missions will perform low-resolution(R$<$100) optical (0.3-1~$\mu$m) spectroscopy of planets, thus enablingreflected spectroscopy of cool giants. Reflected light spectroscopy is encodedwith rich information about the scattering and absorbing properties of planetatmospheres. Given the diversity of clouds and hazes expected in exoplanets, itis imperative we solidify the methodology to accurately and precisely retrievethese scattering and absorbing properties that are agnostic to cloud species.In particular, we focus on determining how different cloud parameterizationsaffect resultant inferences of both cloud and atmospheric composition. Wesimulate mock observations of the reflected spectra from three top prioritydirect imaging cool giant targets with different effective temperatures,ranging from 135 K to 533 K. We perform retrievals of cloud structure andmolecular abundances on these three planets using four differentparameterizations, each with increasing levels of cloud complexity. We findthat the retrieved atmospheric and scattering properties strongly depend on thechoice of cloud parameterization. For example, parameterizations that are toosimplistic tend to overestimate the abundances. Overall, we are unable toretrieve precise/accurate gravity beyond $\pm$50\%. Lastly, we find that evenlow SNR=5, low R=40 reflected light spectroscopy gives cursory zeroth orderinsights into cloud deck position relative to molecular and Rayleigh opticaldepth level.

Cloud Parameterizations and their Effect on Retrievals of Exoplanet Reflection Spectroscopy