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It remains to be ascertained whether sub-Neptune exoplanets primarily possesshydrogen-rich atmospheres or whether a population of H$_2$O-rich "water worlds"lurks in their midst. Addressing this question requires improved modeling ofwater-rich exoplanetary atmospheres, both to predict and interpretspectroscopic observations and to serve as upper boundary conditions oninterior structure calculations. Here we present new models ofhydrogen-helium-water atmospheres with water abundances ranging from solar to100% water vapor. We improve upon previous models of high water contentatmospheres by incorporating updated prescriptions for water self-broadeningand a non-ideal gas equation of state. Our model grid(https://umd.box.com/v/water-worlds) includes temperature-pressure profiles inradiative-convective equilibrium, along with their associated transmission andthermal emission spectra. We find that our model updates primarily act at highpressures, significantly impacting bottom-of-atmosphere temperatures, withimplications for the accuracy of interior structure calculations. Upperatmosphere conditions and spectroscopic observables are less impacted by ourmodel updates, and we find that under most conditions, retrieval codes builtfor hot Jupiters should also perform well on water-rich planets. Weadditionally quantify the observational degeneracies among both thermalemission and transmission spectra. We recover standard degeneracies with cloudsand mean molecular weight for transmission spectra, and we find thermalemission spectra to be more readily distinguishable from one another in thewater-poor (i.e. near-solar) regime.

Where are the Water Worlds?: Self-Consistent Models of Water-Rich Exoplanet Atmospheres