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

TL;DR

This study evaluates the detectability of various atmospheric molecules on transiting terrestrial exoplanets around M dwarfs using ground-based ELT spectroscopy, highlighting the potential to identify habitability indicators and biosignatures.

Contribution

It provides the first comprehensive simulation of high-resolution spectra including systematic effects for multiple molecules across different ELT configurations and planetary atmospheres.

Findings

CH$_4$ and CO$_2$ are most detectable with ELTs.

O$_2$ and H$_2$O bands may be accessible with more observation time.

ELTs can probe atmospheres of planets around earlier-type M dwarfs, surpassing JWST capabilities.

Abstract

Within the next decade, atmospheric O$_2$ on Earth-like M dwarf planets may be accessible with visible--near-infrared, high spectral resolution extremely large ground-based telescope (ELT) instruments. However, the prospects for using ELTs to detect environmental properties that provide context for O$_2$ have not been thoroughly explored. Additional molecules may help indicate planetary habitability, rule out abiotically generated O$_2$, or reveal alternative biosignatures. To understand the accessibility of environmental context using ELT spectra, we simulate high-resolution transit transmission spectra of previously-generated evolved terrestrial atmospheres. We consider inhabited pre-industrial and Archean Earth-like atmospheres, and lifeless worlds with abiotic O$_2$ buildup from CO$_2$ and H$_2$O photolysis. All atmospheres are self-consistent with M2V--M8V dwarf host stars. Our simulations include explicit treatment of systematic and telluric effects to model high-resolution spectra for GMT, TMT, and E-ELT configurations for systems 5 and 12 pc from Earth. Using the cross-correlation technique, we determine the detectability 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 of M 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 observation time. Although this technique still faces considerable challenges, the ELTs will provide access to the atmospheres of terrestrial planets transiting earlier-type M-dwarf hosts that may not be possible using JWST.