Molecular Cross Sections for High Resolution Spectroscopy of Super Earths, Warm Neptunes and Hot Jupiters

High resolution spectroscopy (HRS) has been used to detect a number of species in the atmospheres of hot Jupiters. Key to such detections is accurately and precisely modelled spectra for cross-correlation against the R\(\gtrsim\)20,000 observations. There is a need for the latest generation of opaci...

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Published in:arXiv.org 2020-04
Main Authors: Gandhi, Siddharth, Brogi, Matteo, Yurchenko, Sergei N, Tennyson, Jonathan, Coles, Phillip A, Webb, Rebecca K, Birkby, Jayne L, Guilluy, Gloria, Hawker, George A, Nikku Madhusudhan, Bonomo, Aldo S, Sozzetti, Alessandro
Format: Article
Language:English
Subjects:
Atmospheric models
Carbon monoxide
Cross-sections
Extrasolar planets
Gas giant planets
High resolution
Jupiter
Planetary atmospheres
Pressure broadening
Spectra
Spectral signatures
Spectrum analysis
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Summary:High resolution spectroscopy (HRS) has been used to detect a number of species in the atmospheres of hot Jupiters. Key to such detections is accurately and precisely modelled spectra for cross-correlation against the R\(\gtrsim\)20,000 observations. There is a need for the latest generation of opacities which form the basis for high signal-to-noise detections using such spectra. In this study we present and make publicly available cross sections for six molecular species, H\(_2\)O, CO, HCN, CH\(_4\), NH\(_3\) and CO\(_2\) using the latest line lists most suitable for low- and high-resolution spectroscopy. We focus on the infrared (0.95-5~\(\mu\)m) and between 500-1500~K where these species have strong spectral signatures. We generate these cross sections on a grid of pressures and temperatures typical for the photospheres of super Earth, warm Neptunes and hot Jupiters using the latest H\(_2\) and He pressure broadening. We highlight the most prominent infrared spectral features by modelling three representative exoplanets, GJ~1214~b, GJ~3470~b and HD~189733~b, which encompass a wide range in temperature, mass and radii. In addition, we verify the line lists for H\(_2\)O, CO and HCN with previous high resolution observations of hot Jupiters. However, we are unable to detect CH\(_4\) with our new cross sections from HRS observations of HD~102195~b. These high accuracy opacities are critical for atmospheric detections with HRS and will be continually updated as new data becomes available.
ISSN:2331-8422
DOI:10.48550/arxiv.2004.04160