Feasibility study on retrieving exoplanetary cloud cover distributions using polarimetry

TL;DR

This study explores the potential of polarimetry to map exoplanetary cloud cover distributions, demonstrating the required measurement precision to retrieve latitudinal cloud information from polarimetric data.

Contribution

It introduces a method to infer exoplanet cloud cover using polarimetry and establishes the polarimetric precision needed for such measurements.

Findings

Latitudinal cloud cover can be inferred at 0.1% polarimetric sensitivity when the planetary signal is isolated.

A precision of 10^{-3} ppm is necessary when stellar flux is included to obtain cloud cover information.

Polarimetry offers a promising avenue for exocartography of exoplanets.

Abstract

Context. As a new growing field, exocartography aims to map the surface features of exoplanets that are beyond the resolution of traditional observing techniques. While photometric approaches have been discussed extensively, polarimetry has received less attention despite its promising prospects. Aims. We demonstrate that the limb polarization of an exoplanetary atmosphere offers valuable insights into its cloud cover distribution. Specifically, we determine an upper limit for the polarimetric precision, which is required to extract information about the latitudinal cloud cover of temperate Jovian planets for scenarios of observations with and without host stars. Methods. To compute the scattered stellar radiation of an exoplanetary atmosphere and to study the polarization at various planetary phase angles, we used the three-dimensional Monte Carlo radiative transfer code POLARIS. Results. When the planetary signal can be measured separately from the stellar radiation, information about the latitudinal cloud cover for polar cap models is accessible at polarimetric sensitivities of $0.1$ %. In contrast, a precision of about $10^{-3}$ ppm is required when the stellar flux is included to gain this information.