CO2-broadening and shift coefficients of sulfur dioxide near 4 µm

Borkov, Yu.G.; Lyulin, O.M.; Petrova, T. M.; Solodov, A. M.; Солодов, А. А.; Deichuli, V. M.; Perevalov, V.I.

doi:10.1016/j.jqsrt.2018.12.030

Cited by 13 publications

(19 citation statements)

References 20 publications

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“…Nevertheless, it was found by Lincowski et al (2021) that the HITRAN2016 CO 2 broadening data of SO 2 were broadly consistent with laboratory results from Bellotti and Steffes (2015). For HITRAN2020, the SO 2 -CO 2 broadening data were updated based on the experimental measurements from Borkov et al (2019) and Ceselin et al (2017). Furthermore, extrapolated (beyond laboratory measurements) broadening, temperature dependence, and line shift values were applied by Dudaryonok and Lavrentieva (2018) to transitions where broadening data were not directly available.…”

Section: Relevant Broadening Parameters In Hitranmentioning

confidence: 80%

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

Skinner,

Hargreaves,

Gordon

2022

Preprint

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The high-resolution transmission molecular spectroscopic database (HITRAN) has recently introduced line-by-line broadening parameters (and their temperature dependence) appropriate for the dominant constituents of planetary atmospheres. The latest version of the database, HITRAN2020, has recently been released and constitutes a large and expansive update. In this work, line shape codes suitable for calculating microwave spectra have been implemented within the HITRAN Application Programming Interface (HAPI). These new additions allow for spectroscopic calculations of microwave absorbing species pertinent to current and future studies of the atmospheres of Jupiter and Venus, and more generally for the atmospheres of gas giants and rocky planets. The inversion spectrum of the NH 3 molecule broadened by H 2 , He and H 2 O dominates the microwave region of Jupiter. Whereas for Venus, accurate spectroscopic data of SO 2 broadened by CO 2 is necessary in order to determine its significance, if any, on the reported detection of PH 3 in the Venusian upper cloud deck. Comparisons have been made to available microwave laboratory opacities and the following results illustrate that HITRAN data can be used in conjunction with HAPI to reproduce the existing experimental measurements and provide reliable calculation of planetary opacities.

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Section: Relevant Broadening Parameters In Hitranmentioning

confidence: 80%

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

Skinner,

Hargreaves,

Gordon

2022

Preprint

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“…For 185,637 transitions (34%) derived from the calculated energy levels the positions accuracy corresponds to the 0.001 -0.01 cm -1 error range. In case of the ( 110)-( 000), ( 011)-( 000), ( 101)-( 000), ( 111)-(010) bands the calculated intensities [72] are substituted by the recent experimental data [74], [75] when available. We estimate the quality of variational intensities as 5-10% on average.…”

Section: So2 (Molecule 9)mentioning

confidence: 99%

“…• 3N9: positions are determined from the upper and lower experimental energy levels, intensities are experimental from [75].…”

Section: So2 (Molecule 9)mentioning

confidence: 99%

The 2020 edition of the GEISA spectroscopic database

Delahaye

Armante

Scott

et al. 2021

Journal of Molecular Spectroscopy

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“…One particular example is SO 2 broadened by CO 2 , where prior to Wilzewski et al (2016) only one measurement for a single transition was available in the literature (Krishnaji 1963) and was recorded in 1963. Whereas following Wilzewski et al (2016), a number of comprehensive studies have appeared (Ceselin et al 2017;Dudaryonok & Lavrentieva 2018;Borkov et al 2019). Such measurements are necessary when making accurate identifications of transitions from different molecules but with similar frequencies, as recently demonstrated with the analysis of possibly blended PH 3 and SO 2 transitions in the atmosphere of Venus (Greaves et al 2020;Villanueva et al 2021;Encrenaz et al 2020;Lincowski et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…CO 2 g values for SO 2 lines are a combination of new experimental measurements(Borkov et al 2019;Ceselin et al 2017) where available, and semiempirical model calculated byDudaryonok & Lavrentieva (2018) based on a revised version of their model. Additionally, extrapolated CO 2 -broadening and temperature-dependence values (as well as line shifts) fromDudaryonok & Lavrentieva (2018) were applied to all other HITRAN2020 SO 2 lines where CO 2 -broadening and shift data were not available.…”

mentioning

confidence: 99%

H₂, He, and CO₂ Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO₂, N₂O, CO, SO₂, OH, OCS, H₂CO, HCN, PH₃, H₂S, and GeH₄

Tan

Skinner²,

Samuels

et al. 2022

ApJS

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In recent years, extended efforts have been made to increase the potential for modeling and interpreting the spectra of planetary atmospheres using the HITRAN database. A significant objective is to provide broadening parameters due to the ambient pressure of He, H2, and CO2 gases. Since hydrogen and helium are the main constituents in the atmospheres of gas giants, and carbon dioxide dominates the atmospheres of many rocky planets, these spectroscopic data are essential for radiative transfer models dedicated to planetary atmospheres. In HITRAN2016, the He-, H2- and CO2-broadening parameters and their temperature dependencies, and in some cases pressure-induced shifts, were added to the line lists of CO, SO2, NH3, HF, HCl, OCS, and C2H2. This work describes a further expansion introduced in the HITRAN2020 edition. In particular, relevant data for the line lists of CO2, N2O, OH, H2CO, HCN, PH3, H2S, and GeH4 were added, while those for CO, SO2, and OCS were revised. The new data are based on the semiempirical models constructed on available and validated experimental measurements and theoretical predictions. These models strongly depend on the extent and quality of the available data. The paper explains how to use the online interface or the HITRAN Application Programming Interface (HAPI) to retrieve these data from the database. Examples of calculating a molecule’s spectra in a mixture of buffer-gases using HAPI are also provided. We also provide a set of Python codes allowing one to populate any line list of corresponding molecules with relevant broadening parameters.

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CO2-broadening and shift coefficients of sulfur dioxide near 4 µm

Cited by 13 publications

References 20 publications

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

The 2020 edition of the GEISA spectroscopic database

H₂, He, and CO₂ Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO₂, N₂O, CO, SO₂, OH, OCS, H₂CO, HCN, PH₃, H₂S, and GeH₄

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CO2-broadening and shift coefficients of sulfur dioxide near 4 µm

Cited by 13 publications

References 20 publications

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

Using HITRAN to Model Opacities for Planetary Atmospheres: Test case of Microwave Spectra of NH$_3$, SO$_2$ and PH$_3$

The 2020 edition of the GEISA spectroscopic database

H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4

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H₂, He, and CO₂ Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO₂, N₂O, CO, SO₂, OH, OCS, H₂CO, HCN, PH₃, H₂S, and GeH₄