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Most of the exoplanets detected up to now transit in front of their hoststars, allowing for the generation of transmission spectra; the study ofexoplanet atmospheres relies heavily upon accurate analysis of these spectra.Recent discoveries mean that the study of atmospheric signals from low-mass,temperate worlds are becoming increasingly common. The observed transit depthin these planets is small and more difficult to analyze. Analysis of simulatedtransmission spectra for two small, temperate planets (GJ 1214 b and K2-18 b)is presented, giving evidence for significant differences in simulated transitdepth when the water vapor continuum is accounted for when compared to modelsomitting it. These models use cross-sections from the CAVIAR lab experiment forthe water self-continuum up to 10,000 cm$^{-1}$; these cross-sections exhibitan inverse relationship with temperature, hence lower-temperature atmospheresare the most significantly impacted. Including the water continuum stronglyaffects transit depths, increasing values by up to 80 ppm, with the differencesfor both planets being detectable with the future space missions Ariel andJWST. It is imperative that models of exoplanet spectra move toward adaptivecross-sections, increasingly optimized for H$_2$O-rich atmospheres. Thisnecessitates including absorption contribution from the water vapor continuuminto atmospheric simulations.

Cross-sections for heavy atmospheres: H$_2$O continuum