The ExoMolOP database: Cross sections and<i>k</i>-tables for molecules of interest in high-temperature exoplanet atmospheres

Chubb, Katy L.; Rocchetto, Marco; Yurchenko, Sergei N.; Min, M.; Waldmann, Ingo; Barstow, Joanna K.; Mollière, P.; Al-Refaie, Ahmed; Phillips, Mark; Tennyson, Jonathan

doi:10.1051/0004-6361/202038350

Cited by 122 publications

(124 citation statements)

References 237 publications

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“…Recently Chubb et al [262] computed opacity cross sections and k -tables for all molecules available from the ExoMol database plus some atomic data from NIST. These data are formatted for use in various retrieval codes including Tau-REx [13][14][15] , ARCiS [24] , petitRADTRANS [28] , and NEMESIS [17] .…”

Section: Exomolop: Opacitiesmentioning

confidence: 99%

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Tennyson

Yurchenko

Al-Refaie

et al. 2020

Journal of Quantitative Spectroscopy and Radiative Transfer

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192

161

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The ExoMol database ( www.exomol.com ) provides molecular data for spectroscopic studies of hot atmospheres. While the data are intended for studies of exoplanets and other astronomical bodies, the dataset is widely applicable. The basic form of the database is extensive line lists; these are supplemented with partition functions, state lifetimes, cooling functions, Landé g-factors, temperature-dependent cross sections, opacities, pressure broadening parameters, k -coefficients and dipoles. This paper presents the latest release of the database which has been expanded to consider 80 molecules and 190 isotopologues totaling over 700 billion transitions. While the spectroscopic data are concentrated at infrared and visible wavelengths, ultraviolet transitions are being increasingly considered in response to requests from observers. The core of the database comes from the ExoMol project which primarily uses theoretical methods, albeit usually fine-tuned to reproduce laboratory spectra, to generate very extensive line lists for studies of hot bodies. The data have recently been supplemented by line lists derived from direct laboratory observations, albeit usually with the use of ab initio transition intensities. A major push in the new release is towards accurate characterisation of transition frequencies for use in high resolution studies of exoplanets and other bodies.

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Section: Exomolop: Opacitiesmentioning

confidence: 99%

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Tennyson

Yurchenko

Al-Refaie

et al. 2020

Journal of Quantitative Spectroscopy and Radiative Transfer

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192

161

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“…Because clouds are most constrained by the transmission spectrum, we model them with a fully opaque cloud layer above a given pressure, restricted to the day-and night-side regions. For the chemistry, we use the molecular line lists from the Exomol project (Tennyson et al 2016(Tennyson et al , 2020Chubb et al 2021), HITEMP (Rothman & Gordon 2014), and HITRAN (Gordon et al 2016) (Li et al 2015), CO 2 (Rothman et al 2010), C 2 H 2 (Wilzewski et al 2016), C 2 H 4 (Mant et al 2018), NH 3 (Yurchenko et al 2011), andHCN (Harris et al 2006;Barber et al 2013).…”

Section: Opacity Sourcesmentioning

confidence: 99%

An Exploration of Model Degeneracies with a Unified Phase Curve Retrieval Analysis: The Light and Dark Sides of WASP-43 b

Changeat

Al-Refaie

Edwards

et al. 2021

ApJ

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The analysis of exoplanetary atmospheres often relies upon the observation of transit or eclipse events. While very powerful, these snapshots provide mainly one-dimensional information on the planet structure and do not easily allow precise latitude-longitude characterizations. The phase curve technique, which consists of measuring the planet emission throughout its entire orbit, can break this limitation and provide useful two-dimensional thermal and chemical constraints on the atmosphere. As of today, however, computing performances have limited our ability to perform unified retrieval studies on the full set of observed spectra from phase curve observations at the same time. Here, we present a new phase curve model that enables fast, unified retrieval capabilities. We apply our technique to the combined phase curve data from the Hubble and Spitzer space telescopes of the hot Jupiter WASP-43 b. We tested different scenarios and discussed the dependence of our solution on different assumptions in the model. Our more comprehensive approach suggests that multiple interpretations of this data set are possible, but our more complex model is consistent with the presence of thermal inversions and a metal-rich atmosphere, contrasting with previous data analyses, although this likely depends on the Spitzer data reduction. The detailed constraints extracted here demonstrate the importance of developing and understanding advanced phase curve techniques, which we believe will unlock access to a richer picture of exoplanet atmospheres.

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“…Knowledge of the absorption signatures of metal hydrides and oxides is informed by their detections in brown dwarfs (e.g. Chubb et al (2021) in order to feed them into TAUREX as part of the ExoMolOP database 3 . In this study, we have used the k-tables with R = ∆λ λ = 300.…”

Section: Taurex IImentioning

confidence: 99%

Evidence for chromium hydride in the atmosphere of hot Jupiter WASP-31b

Braam

Tak

Chubb

et al. 2021

A&A

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Context. The characterisation of exoplanet atmospheres has shown a wide diversity of compositions. Hot Jupiters have the appropriate temperatures to host metallic compounds, which should be detectable through transmission spectroscopy. Aims. We aim to detect exotic species in the transmission spectra of hot Jupiters, specifically WASP-31b, by testing a variety of chemical species to explain the spectrum. Methods. We conduct a re-analysis of publicly available transmission data of WASP-31b using the Bayesian retrieval framework TAUREX II. We retrieve various combinations of the opacities of 25 atomic and molecular species to determine the minimum set that is needed to fit the observed spectrum. Results. We report evidence for the spectroscopic signatures of chromium hydride (CrH), H2O, and K in WASP-31b. Compared to a flat model without any signatures, a CrH-only model is preferred with a statistical significance of ~3.9σ. A model consisting of both CrH and H2O is found with ~2.6 and ~3σ confidence over a CrH-only model and an H2O-only model, respectively. Furthermore, weak evidence for the addition of K is found at ~2.2σ over the H2O+CrH model, although the fidelity of the data point associated with this signature was questioned in earlier studies. Finally, the inclusion of collision-induced absorption and a Rayleigh scattering slope (indicating the presence of aerosols) is found with ~3.5σ confidence over the flat model. This analysis presents the first evidence for signatures of CrH in a hot Jupiter atmosphere. At a retrieved temperature of 1481−355+264 K, the atmosphere of WASP-31b is hot enough to host gaseous Cr-bearing species, and the retrieved abundances agree well with predictions from thermal equilibrium chemistry. Furthermore, the retrieved abundance of CrH agrees with the abundance in an L-type brown dwarf atmosphere. However, additional retrievals using VLT FORS2 data lead to a non-detection of CrH. Future observations with James Webb Space Telescope have the potential to confirm the detection and/or discover other CrH features.

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The ExoMolOP database: Cross sections andk-tables for molecules of interest in high-temperature exoplanet atmospheres

Cited by 122 publications

References 237 publications

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

An Exploration of Model Degeneracies with a Unified Phase Curve Retrieval Analysis: The Light and Dark Sides of WASP-43 b

Evidence for chromium hydride in the atmosphere of hot Jupiter WASP-31b

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