Using near infra-red spectroscopy for characterization of transiting exoplanets

TL;DR

This paper introduces a high-precision near-infrared spectroscopic method for characterizing exoplanet atmospheres, capable of identifying key molecules in both large and small transiting planets using existing telescope technology.

Contribution

It presents a novel inverse analysis technique combining stellar and telluric models to accurately recover exoplanet transmission spectra across a wide near-infrared range.

Findings

Method can detect molecules like O2, CH4, CO2, H2O in exoplanet atmospheres.

Achieves sufficient accuracy with 8m telescopes for Jupiter-size planets.

Potential to characterize smaller rocky planets with fewer transits.

Abstract

We propose a method for observing transiting exoplanets with near-infrared high-resolution spectrometers. We aim to create a robust data analysis method for recovering atmospheric transmission spectra from transiting exoplanets over a wide wavelength range in the near infrared. By using an inverse method approach, combined with stellar models and telluric transmission spectra, the method recovers the transiting exoplanet's atmospheric transmittance at high precision over a wide wavelength range. We describe our method and have tested it by simulating observations. This method is capable of recovering transmission spectra of high enough accuracy to identify absorption features from molecules such as O2, CH4, CO2, and H2O. This accuracy is achievable for Jupiter-size exoplanetsat S/N that can be reached for 8m class telescopes using high-resolution spectrometers (R>20 000) during a single transit, and for Earth-size planets and super-Earths transiting late K or M dwarf stars at S/N reachable during observations of less than 10 transits. We also analyse potential error sources to show the robustness of the method. Detection and characterization of atmospheres of both Jupiter-size planets and smaller rocky planets looks promising using this set-up.