Model-independent exoplanet transit spectroscopy

TL;DR

This paper introduces a novel, model-independent data analysis method for exoplanet transit spectroscopy that simultaneously recovers planetary atmospheres and stellar intensities directly from light curves, improving robustness and fidelity.

Contribution

The method allows for model-independent extraction of exoplanet transmission spectra and stellar intensities, removing reliance on theoretical stellar and planetary models.

Findings

Successfully reproduces results of quadratic limb darkening models

Effectively eliminates spurious features caused by telluric absorption

Accurately reconstructs stellar specific intensity from observational data

Abstract

We propose a new data analysis method for obtaining transmission spectra of exoplanet atmospheres and brightness variation across the stellar disk from transit observations. The new method is capable of recovering exoplanet atmosphere absorption spectra and stellar specific intensities without relying on theoretical models of stars and planets. We fit both stellar specific intensity and planetary radius simultaneously directly to transit light curves. This allows stellar models to be removed from the data analysis. Furthermore, we use a data-quality weighted filtering technique to achieve an optimal trade-off between spectral resolution and reconstruction fidelity homogenising the signal to noise ratio across the wavelength range. Such approach is more efficient than conventional data binning onto a low resolution wavelength grid. We demonstrate that our analysis is capable of re-producing results achieved by using explicit quadratic limb darkening equation, and that the filtering technique helps eliminating spurious spectral features in regions with strong telluric absorption. The method is applied to the VLT FORS2 observations of the exoplanets GJ 1214 b and WASP-49 b, and our results are in agreement with previous studies. Comparisons between obtained stellar specific intensity and numerical models indicates that the method is capable of accurately reconstructing the specific intensity. The proposed method enables more robust characterization of exoplanetary atmospheres by separating derivation of planetary transmission and stellar specific intensity spectra (that is model-independent) from chemical and physical interpretation.