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Understanding the limits of rocky planet habitability is one of the key goalsof current and future exoplanet characterization efforts. An intrinsic conceptof rocky planet habitability is the Habitable Zone. To date, the most widelyused estimates of the Habitable Zone are based on cloud-free, one-dimensional(vertical) radiative-convective climate model calculations. However, recentthree-dimensional global climate modeling efforts have revealed that rockyplanet habitability is strongly impacted by radiative cloud feedbacks, wherecomputational expense and model limitations can prevent these tools fromexploring the limits of habitability across the full range of parameter space.We leverage a patchy cloud one-dimensional radiative-convective climate modelwith parameterized cloud microphysics to investigate Inner Edge limits to theHabitable Zone for main sequence stars ($T_{\rm eff}$ = 2600 -7200K). We findthat Inner Edge limits to the Habitable Zone can be 3.3 and 4.7 times closerthan previous cloud-free estimates for Earth- and super-Earth-sized worlds,respectively, depending on bulk cloud parameters (e.g., fractional cloudinessand sedimentation efficiency). These warm, moist Inner Edge climates areexpected to have extensive cloud decks that could mute deep atmosphere spectralfeatures. To aid in rocky planet characterization studies, we identify thepotential of using $\rm{CO_{\rm 2}}$ absorption features in transmissionspectroscopy as a means of quantifying cloud deck height and cloudsedimentation efficiency. Moist greenhouse climates may represent key yetpoorly understood states of habitable planets for which continued study willuncover new insights into the search and characterization of habitable worlds.

Inner Edge Habitable Zone Limits Around Main Sequence Stars: Cloudy Estimates