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We present a transmission spectrum for the warm (500-600K) sub-NeptuneHD3167c obtained using the Hubble Space Telescope Wide Field Camera 3 infraredspectrograph. We combine these data, which span the 1.125-1.643 micronwavelength range, with broadband transit measurements made using Kepler/K2(0.6-0.9 micron) and Spitzer/IRAC (4-5 micron). We find evidence for absorptionby at least one of H2O, HCN, CO2, and CH4 (Bayes factor 7.4; 2.5-sigmasignificance), although the data precision does not allow us to unambiguouslydiscriminate between these molecules. The transmission spectrum rules outcloud-free hydrogen-dominated atmospheres with metallicities <100x solar at>5.8-sigma confidence. In contrast, good agreement with the data is obtainedfor cloud-free models assuming metallicities >700x solar. However, forretrieval analyses that include the effect of clouds, a much broader range ofmetallicities (including subsolar) is consistent with the data, due to thedegeneracy with cloud-top pressure. Self-consistent chemistry models thataccount for photochemistry and vertical mixing are presented for the atmosphereof HD3167c. The predictions of these models are broadly consistent with ourabundance constraints, although this is primarily due to the largeuncertainties on the latter. Interior structure models suggest the core massfraction is >40%, independent of a rock or water core composition, andindependent of atmospheric envelope metallicity up to 1000x solar. We alsoreport abundance measurements for fifteen elements in the host star, showingthat it has a very nearly solar composition.

Transmission spectroscopy for the warm sub-Neptune HD3167c: evidence for molecular absorption and a possible high metallicity atmosphere