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Escaping exoplanet atmospheres have been observed as deep transit signaturesin a few specific spectral lines. Detections have been made in the hydrogenLy-$\alpha$ line, the metastable helium line at 10830 {\AA} and some UV linesof metallic species. Observational challenges, unexpected non-detections andmodel degeneracies have generally made it difficult to draw definitiveconclusions about the escape process for individual planets. Expanding on thesuite of spectral tracers used may help to mitigate these challenges. Wepresent a new framework for modeling the transmission spectrum ofhydrodynamically escaping atmospheres. We predict FUV to NIR spectra forsystems with different planet and stellar types and identify new lines that canpotentially be used to study their upper atmospheres. Measuring the radius inthe atmosphere at which the strongest lines form puts them into context withinthe upper atmospheric structure. Targeting a set of complementary spectrallines for the same planet will help us to better constrain the outflowproperties.

Expanding the inventory of spectral lines used to trace atmospheric escape in exoplanets