ИСТИНА

The recently released 2020 edition of the HITRAN database, available from HITRANonline (www.hitran.org), includes several types of spectroscopic data essential to remote sensing of planetary atmospheres. HITRAN2020 significantly improves on previous editions [1], and an emphasis has been placed on expanding the spectroscopic data of relevance to a variety of planetary atmospheres, including giant planets and Titan. This presentation will highlight significant improvements of relevant spectroscopy in HITRAN and will address the remaining deficiencies. The HITRAN2020 line-by-line section encompasses 144 isotopologues of 55 molecular species, and many of these molecules are present in the atmospheres of Jupiter, Saturn, and Titan. For instance, the line lists for H2O, CH4, NH3, PH3, C2H6, (and more) have benefitted from extended spectral coverage, additional vibrational bands, increased parameter accuracy, and improved band-to-band consistency. Six new line-by-line molecules have been added for HITRAN2020, including germane (GeH4). Moreover, the SQL database structure enables numerous additional parameters to be provided alongside the traditional ".par" format. This allows for increased applicability toward giant planet atmospheres via the inclusion of H2, He, and/or H2O broadening parameters, which are now available in HITRAN for 19 molecules [2,3]. In addition to line-by-line data, numerous experimental absorption cross-sections are also available at HITRANonline for over 320 molecular species. Many absorption cross-sections have been added for HITRAN2020, which for the first time includes measurements at low (down to 145 K) and high (up to 773 K) temperatures for the same molecule (e.g., propane). Spectral coverage, resolution, pressure, and broadening gas have also been extended for several molecules. For instance, cross-sections for several hydrocarbons (e.g., ethane, propene, propane, isobutene) now include H2-, He-, and/or N2-broadening. Furthermore, the collision-induced absorption (CIA) data for a variety of relevant collision pairs has been updated [4,5]. This work is supported through the NASA grant 80NSSC20K1059. [1] Gordon, et al., (2017), JQSRT 203, 3. [2] Tan, et al., (2019), JGR-Atmos. 124, 11580. [3] Tan, et al., (2021), in prep. [4] Karman et al. ,(2019) Icarus, 328, 160 [5] Chistikov, et al., (2019), J Phys. Chem. 151, 194106.