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The search for water-rich Earth-sized exoplanets around low-mass stars israpidly gaining attention because they represent the best opportunity tocharacterize habitable planets in the near future. Understanding theatmospheres of these planets and determining the optimal strategy forcharacterizing them through transmission spectroscopy with our upcominginstrumentation is essential in order to constrain their environments. For thisstudy, we present simulated transmission spectra of tidally locked Earth-sizedocean-covered planets around late-M to mid-K stellar spectral types, utilizingGCM modeling results previously published by Kopparapu et al. (2017) as inputsfor our radiative transfer calculations performed using NASA's PlanetarySpectrum Generator (psg.gsfc.nasa.gov; Villanueva et al. (2018)). We identifytrends in the depth of H$_2$O spectral features as a function of planet surfacetemperature and rotation rate. These trends allow us to calculate the exposuretimes necessary to detect water vapor in the atmospheres of aquaplanets throughtransmission spectroscopy with the upcoming James Webb Space Telescope (JWST)as well as several future flagship space telescope concepts under consideration(LUVOIR and OST) for a target list constructed from the TESS Input Catalog(TIC). Our calculations reveal that transmission spectra for water-richEarth-sized planets around low-mass stars will be dominated by clouds, withspectral features < 20 ppm, and only a small subset of TIC stars would allowfor the characterization of an ocean planet in the Habitable Zone. We thuspresent a careful prioritization of targets that are most amenable to follow-upcharacterizations with next-generation instrumentation, in order to assist thecommunity in efficiently utilizing precious telescope time.

Dim Prospects for Transmission Spectra of Ocean Earths Around M Stars