A high-accuracy computed water line list

By R. Barber, Jonathan Tennyson, G. J. Harris, R. Tolchenov. 2006

616 citations recorded by the source corpus.

A computed list of H2 16 O infrared transition frequencies and intensities is presented. The list, BT2, was produced using a discrete variable representation two-step approach for solving the rotation‐vibration nuclear motions. It is the most complete water line list in existence, comprising over 500 million transitions (65 per cent more than any other list) and it is also the most accurate (over 90 per cent of all known experimental energy levels are within 0.3 cm −1 of the BT2 values). Its accuracy has been confirmed by extensive testing against astronomical and laboratory data. The line list has been used to identify individual water lines in a variety of objects including comets, sunspots, a brown dwarf and the nova-like object V838 Mon. Comparison of the observed intensities with those generated by BT2 enables water abundances and temperatures to be derived for these objects. The line list can also be used to provide an opacity for models of the atmospheres of M dwarf stars and assign previously unknown water lines in laboratory

Subfields: Atmospheric Science, Global and Planetary Change, Spectroscopy

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Citations in the corpus

New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit (2015, methodology): “This stems from the use of the more complete and accurate water linelist of Barber et al. (2006), compared to previously used ones, namely Miller et al. (1994) in NextGen and Partridge & Schwenke (1997) in Dusty/Cond.”
MARVEL: Measured active rotational–vibrational energy levels. II. Algorithmic improvements☆ (2012, background): “The (sufficiently) complete linelist information about allowed transitions, corresponding to very large SNs, can only be determined via sophisticated variational rotational– vibrational computations [31].”
The effective temperature scale of M dwarfs (2013, methodology): “But for over ten years already, water vapor (Partridge & Schwenke 1997, Barber et al. 2006) and titanium oxide (Plez 1998) line lists, the two most important opacities in strength and spectral coverage, have become available meeting these conditions.”
The 2015 edition of the GEISA spectroscopic database (2016, neutral): “787 191846 534227 405919 50633 13515 4393851 6197 105079 83668 104223 46414 20364 691161 42866 107 533 1293 806 7230 33809 44611 53803 58763 12969 53227 824 138103 8983 71954 417540 179347 17862 120 83043 126983 58650 62684 70904 92398 -18 -18 -20 -17 -18 -19 -24 -19 -20 -18 -19 -18 -20 -16 -16 -18 ”
ExoMol line lists IV: The rotation-vibration spectrum of methane up to 1500 K (2014, background): “Its construction means that there are now hot line lists for the key set of molecules methane, water (Barber et al. 2006) and ammonia (Yurchenko, Barber & Tennyson 2011b).”
Transit spectrophotometry of the exoplanet HD189733b. I. Searching for water but finding haze with HST NICMOS (2009, methodology): “87=1.79×10 −21 (cm2 molecule−1), respectively, using the high temperature line list of Barber et al. (2006), a Voigt broadening line profile, a temperature of 1200 K, and the response through our two narrowband filters.”
ExoMol molecular line lists XXX: a complete high-accuracy line list for water (2018, methodology): “For infrared frequencies and temperatures up to 2000 K the overall absorption modelled by POKAZATEL is very similar to the one by BT2 (Barber et al. 2006), although the accuracy of individual lines is significantly improved as illustrated by Tables 1 and 2.”
The ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2016, neutral): “[178] ExoMol NH3 2 c 1500 1 1 138 323 351 BYTe Yurchenko et al.”
HITEMP, the high-temperature molecular spectroscopic database (2010, methodology): “[4]) accompanied with a negative sign was used.”
Total internal partition sums for 166 isotopologues of 51 molecules important in planetary atmospheres: Application to HITRAN2016 and beyond (2017, methodology): “The TIPS agree with the reported UCL (University College London) data [31], which are reported to 3000 K.”
The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2020, neutral): “[178] ExoMol NH3 2 c 1500 1 1 138 323 351 BYTe Yurchenko et al.”
A Population Study of Gaseous Exoplanets (2017, methodology): “We hence restricted further retrievals to a smaller set of molecules: H2O (Barber et al. 2006), CO (Rothman et al. 2010), CO2 (Rothman et al. 2010), CH4 (Yurchenko & Tennyson 2014) and NH3 (Yurchenko et al. 2011).”
ExoMol: molecular line lists for exoplanet and other atmospheres (2012, methodology): “This can be done by comparing the ratio of the partition function computed by summing over all lower-state energy levels used to compute the line list to the accurate partition function (Neale et al. 1996; Barber et al. 2006).”
CLOUDS AND CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HR8799b (2011, background): “…with a new, more robust and chemically complete, equation of state3, a revised treatment of pure dust grains, improved alkali line profiles (Allard et al. 2007), and new molecular line lists, most notably for methane (Warmbier et al. 2009; Hauschildt et al. 2009) and water (Barber et al. 2006).”