The ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

By Jonathan Tennyson, Sergei N. Yurchenko, Ahmed Alrefaie, Victoria H J Clark, Katy L. Chubb, E. Conway, Akhil Dewan, Maire N Gorman, C. Hill, A. Lynas-Gray and 12 more. 2016

388 citations recorded by the source corpus.

The ExoMol database (www.exomol.com) provides extensive line lists of molecular transitions which are valid over extended temperature ranges. The status of the current release of the database is reviewed and a new data structure is specified. This structure augments the provision of energy levels (and hence transition frequencies) and Einstein A coefficients with other key properties, including lifetimes of individual states, temperature-dependent cooling functions, Lande g-factors, partition functions, cross sections, k-coefficients and transition dipoles with phase relations. Particular attention is paid to the treatment of pressure broadening parameters. The new data structure includes a definition file which provides the necessary information for utilities accessing ExoMol through its application programming interface (API). Prospects for the inclusion of new species into the database are discussed.

Subfields: Atmospheric Science, Atomic and Molecular Physics, and Optics, Spectroscopy

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Citations in the corpus

HD 209458b in new light: evidence of nitrogen chemistry, patchy clouds and sub-solar water (2017, methodology): “We use the latest theoretical and experimental line lists available, drawing from the HITEMP database for H2O, CO and CO2 (Rothman et al. 2010) and EXOMOL for CH4, HCN and NH3 (Tennyson et al. 2016).”
H2O abundances and cloud properties in ten hot giant exoplanets (2018, methodology): “In particular, our CH4, HCN, and NH3 molecular line data are from EXOMOL (Tennyson et al. 2016; Yurchenko et al. 2011; Barber et al. 2014; Yurchenko & Tennyson 2014) and the line data for H2O, CO, and CO2 are obtained from HITEMP (Rothman et al. 2010).”
ExoMol molecular line lists – XXXV. A rotation-vibration line list for hot ammonia (2019, methodology): “We note that at the moment the format used by the ExoMol data base (Tennyson, Hill & Yurchenko 2013; Tennyson et al. 2016) does not distinguish between those transitions that are reproduced with experimental accuracy and those that are the result of theoretical predictions.”
An Accurate, Extensive, and Practical Line List of Methane for the HITEMP Database (2020, background): “…hot bands and high-J transitions have been included in global variational CH4 line lists : ‘10to10’ (Yurchenko & Tennyson 2014), as part of the ExoMol project (Tennyson et al. 2016), and the Rey et al. (2014a) line list (referred to here as RNT2014) as a part of TheoReTS project (Rey et al. 2016).”
A Population Study of Gaseous Exoplanets (2017, methodology): “This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 758892, ExoAI) and under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ ERC grant agreement numbers 617119 (ExoL”
ExoMol molecular line lists XXX: a complete high-accuracy line list for water (2018, neutral): “All data, including pressure broadening ones, can be found in the ExoMol database (Tennyson et al. 2016). c© 2017 RAS, MNRAS 000, 1–16 c© 2017 RAS, MNRAS 000, 1–16”
The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2020, background): “ExoMol line lists have been published as a series in the journal Monthly Notices of the Royal Astronomical Society (see below) and a first data release in 2016 [62], henceforth ExoMol2016, provided full documentation for the ExoMol database which can be found at www.”
ExoMol molecular line lists – XXXIII. The spectrum of Titanium Oxide (2019, methodology): “…active space was identical to Langhoff (1997), as was the icMRCI methodology (for completeness, we note that the value of n in icMRCI(n) notation introduced in Tennyson et al. (2016a) is equal to one plus the number of states with the same C∞v spin symmetry lower in energy than the target state).”