# The O2 A-band in fluxes and polarization of starlight reflected by Earth-like exoplanets

## TL;DR

This study analyzes how surface and cloud properties affect the O2 A-band in flux and polarization spectra of Earth-like exoplanets, aiding in the detection of atmospheric biosignatures.

## Contribution

It provides a detailed investigation of how surface albedo, cloud optical thickness, altitude, and O2 mixing ratio influence the O2 A-band in reflected light spectra.

## Key findings

- Cloud properties significantly impact the O2 A-band strength.
- Flux and polarization measurements together help reduce degeneracies.
- High temporal and phase angle observations improve atmospheric characterization.

## Abstract

Earth-like, potentially habitable exoplanets are prime targets in the search for extraterrestrial life. Information about their atmosphere and surface can be derived by analyzing light of the parent star reflected by the planet. We investigate the influence of the surface albedo $A_{\rm s}$, the optical thickness $b_{\rm cloud}$ and altitude of water clouds, and the mixing ratio $\eta$ of biosignature O$_2$ on the strength of the O$_2$ A-band (around 760 nm) in flux and polarization spectra of starlight reflected by Earth-like exoplanets. Our computations for horizontally homogeneous planets show that small mixing ratios ($\eta$ < 0.4) will yield moderately deep bands in flux and moderate to small band strengths in polarization, and that clouds will usually decrease the band depth in flux and the band strength in polarization. However, cloud influence will be strongly dependent on their properties such as optical thickness, top altitude, particle phase, coverage fraction, horizontal distribution. Depending on the surface albedo, and cloud properties, different O$_2$ mixing ratios $\eta$ can give similar absorption band depths in flux and band strengths in polarization, in particular if the clouds have moderate to high optical thicknesses. Measuring both the flux and the polarization is essential to reduce the degeneracies, although it will not solve them, in particular not for horizontally inhomogeneous planets. Observations at a wide range of phase angles and with a high temporal resolution could help to derive cloud properties and, once those are known, the mixing ratio of O$_2$ or any other absorbing gas.