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Within the next decade, atmospheric O$_2$ on Earth-like M dwarf planets maybe accessible with visible--near-infrared, high spectral resolution extremelylarge ground-based telescope (ELT) instruments. However, the prospects forusing ELTs to detect environmental properties that provide context for O$_2$have not been thoroughly explored. Additional molecules may help indicateplanetary habitability, rule out abiotically generated O$_2$, or revealalternative biosignatures. To understand the accessibility of environmentalcontext using ELT spectra, we simulate high-resolution transit transmissionspectra of previously-generated evolved terrestrial atmospheres. We considerinhabited pre-industrial and Archean Earth-like atmospheres, and lifelessworlds with abiotic O$_2$ buildup from CO$_2$ and H$_2$O photolysis. Allatmospheres are self-consistent with M2V--M8V dwarf host stars. Our simulationsinclude explicit treatment of systematic and telluric effects to modelhigh-resolution spectra for GMT, TMT, and E-ELT configurations for systems 5and 12 pc from Earth. Using the cross-correlation technique, we determine thedetectability of major species in these atmospheres: O$_2$, O$_3$, CH$_4$,CO$_2$, CO, H$_2$O, and C$_2$H$_6$. Our results suggest that CH$_4$ and CO$_2$are the most accessible molecules for terrestrial planets transiting a range ofM dwarf hosts using an E-ELT, TMT, or GMT sized telescope, and that the O$_2$NIR and H$_2$O 0.9 $\mu$m bands may also be accessible with more observationtime. Although this technique still faces considerable challenges, the ELTswill provide access to the atmospheres of terrestrial planets transitingearlier-type M-dwarf hosts that may not be possible using JWST.

There's more to life than O$_2$: Simulating the detectability of a range  of molecules for ground-based high-resolution spectroscopy of transiting  terrestrial exoplanets