Toward Robust Corrections for Stellar Contamination in JWST Exoplanet Transmission Spectra

TL;DR

This paper investigates the challenges of correcting stellar contamination in JWST exoplanet transmission spectra, emphasizing the importance of high-fidelity stellar models and proposing data-driven and empirical methods for improved correction.

Contribution

It assesses the reliability of stellar models for contamination correction, highlights the impact of model discrepancies, and advocates for data-driven and empirical approaches to enhance correction accuracy.

Findings

Discrepancies between stellar models significantly affect noise levels.

High-fidelity models enable accurate retrieval of stellar photospheric components.

Stellar contamination noise is below photon noise in optimal conditions.

Abstract

Transmission spectroscopy is still the preferred characterization technique for exoplanet atmospheres, although it presents unique challenges that translate into characterization bottlenecks when robust mitigation strategies are missing. Stellar contamination is one such challenge that can overpower the planetary signal by up to an order of magnitude, and thus not accounting for it can lead to significant biases in the derived atmospheric properties. Yet this accounting may not be straightforward, as important discrepancies exist between state-of-the-art stellar models and measured spectra and between models themselves. Here we explore the extent to which stellar models can be used to reliably correct for stellar contamination and yield a planet's uncontaminated transmission spectrum. We find that discrepancies between stellar models can significantly contribute to the noise budget of JWST transmission spectra of planets around stars with heterogeneous photospheres, the true number of unique photospheric spectral components and their properties can only be accurately retrieved when the stellar models have sufficient fidelity, and under such optimistic circumstances the contribution of stellar contamination to the noise budget of a transmission spectrum is considerably below that of the photon noise for the standard transit observation setup. Therefore, we advocate for further development of model spectra of stars and their active regions in a data-driven manner, empirical approaches for deriving spectra of photospheric components using the observatories with which the atmospheric explorations are carried out, and analysis techniques accounting for multimodal posterior distributions for photospheric parameters of interest, which will be increasingly revealed by precise JWST measurements.