Authors

I. E. Gordon, Center for Astrophysics/Harvard & Smithsonian
L. S. Rothman, Center for Astrophysics/Harvard & Smithsonian
R. J. Hargreaves, Center for Astrophysics/Harvard & Smithsonian
F. M. Gomez, Center for Astrophysics/Harvard & Smithsonian
T. Bertin, Center for Astrophysics/Harvard & Smithsonian
C. Hill, Vienna International Centre
R. V. Kochanov, Russian Academy of Sciences
Y. Tan, University of Science and Technology of China
P. Wcisło, Nicolaus Copernicus University of Torun
V. Yu. Makhnev, Center for Astrophysics/Harvard & Smithsonian
P. F. Bernath, Old Dominion UniversityFollow
M. Birk, German Aerospace Center (DLR), Remote Sensing Technology Institute
V. Boudon, Université Bourgogne Europe
A. Campargue, University of Grenoble Alpes
A. Coustenis, Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Paris Observatory
B. J. Drouin, California Institute of Technology
R. R. Gamache, University of Massachusetts Lowell
J. T. Hodges, National Institute of Standards and Technology, Material Measurement Laboratory
D. Jacquemart, Sorbonne Université
E. J. Mlawer, Atmospheric and Environmental Research, Lexington MA
A. V. Nikitin, Technion - Israel Institute of Technology
V. I. Perevalov, Russian Academy of Sciences
M. Rotger, Groupe de Spectrométrie Moléculaire et Atmosphérique
S. Robert, Royal Belgian Institute for Space Aeronomy (BIRA-IASB)
J. Tennyson, University College London
G. C. Toon, California Institute of Technology
H. Tran, Sorbonne Université
V. G. Tyuterev, Russian Academy of Sciences
E. M. Adkins, National Institute of Standards and Technology, Material Measurement Laboratory
A. Barbe, Groupe de Spectrométrie Moléculaire et Atmosphérique, UMR CNRS 7331
D. M. Bailey, National Institute of Standards and Technology, Material Measurement Laboratory
K. Bielska, Nicolaus Copernicus University in Torun
L. Bizzocchi, Università di Bologna
T. A. Blake, Pacific Northwest National Laboratory
C. A. Bowesman, University College London
P. Cacciani, Univ. Lille, CNRS, UMR 8523 - PhLAM - Physique des Lasers, Atomes et Molécules
P. Čermák, Comenius University in Bratislava
A. G. Császár, Loránd University
L. Denis, Center for Astrophysics/Harvard & Smithsonian
S. C. Egbert, University of Colorado Boulder
O. Egorov, Russian Academy of Sciences
A. Yu. Ermilov, Lomonosov Moscow State University
A. J. Fleisher, Material Measurement Laboratory
H. Fleurbaey, University of Grenoble Alpes
A. Foltynowicz, Umeå University
T. Furtenbacher, ELTE Eötvös Loránd University
M. Germann, Umeå University
E. R. Guest, University College London, London
J. J. Harrison, Space Park Leicester
J. -M. Hartmann, Sorbonne Université
A. Hjältén, Umeå University
S. -M. Hu, University of Science and Technology of China
X. Huang, SETI Institute
T. J. Johnson, Pacific Northwest National Laboratory
H. Jóźwiak, Nicolaus Copernicus University in Torun
S. Kassi, University of Grenoble Alpes
M. V. Khan, Sorbonne Université
F. Kwabia-Tchana, Université Paris Cité and Univ. Paris Est Creteil
T. J. Lee, NASA Ames Research Center
D. Lisak, Nicolaus Copernicus University in Torun
A. -W. Liu, University of Science and Technology of China, Hefei, China
O. M. Lyulin, Russian Academy of Sciences
N. A. Malarich, University of Colorado Boulder
L. Manceron, Synchrotron SOLEIL, Beamline AILES
A. A. Marinina, Russian Academy of Sciences
S. T. Massie, University of Colorado
J. Mascio, Atmospheric and Environmental Research, Lexington MA
E. S. Medvedev, Russian Academy of Sciences
V. V. Meshkov, Lomonosov Moscow State University
G. Ch. Mellau, Justus-Liebig-Universität Giessen
M. Melosso, Università di Bologna
S. N. Mikhailenko, Russian Academy of Sciences
D. Mondelain, University of Grenoble Alpes
H.S.P. Müller, Universität zu Köln
M. O' Donnell, Center for Astrophysics/Harvard & Smithsonian
A. Owens, University College London
A. Perrin, Sorbonne Université
O. L. Polyansky, University College London
P. L. Raston, University of Hawai’i at Mānoa
Z. D. Reed, National Institute of Standards and Technology, Material Measurement Laboratory
M. Rey, Groupe de Spectrométrie Moléculaire et Atmosphérique
C. Richard, Laboratoire Interdisciplinaire Carnot de Bourgogne ICB UMR 6303
G. B. Rieker, University of Colorado Boulder
C. Röske, Remote Sensing Technology Institute, Wessling, Germany
S. W. Sharpe, Pacific Northwest National Laboratory
E. Starikova, Russian Academy of Sciences
N. Stolarczyk, Nicolaus Copernicus University in Torun
A. V. Stolyarov, Lomonosov Moscow State University
K. Sung, California Institute of Technology
F. Tamassia, Università di Bologna
J. Terragni, NASA Goddard Space Flight Center
V. G. Ushakov, Russian Academy of Sciences
S. Vasilchenko, Russian Academy of Sciences
B. Vispoel, Royal Belgian Institute for Space Aeronomy (BIRA-IASB)
K. L. Vodopyanov, University of Central Florida
G. Wagner, Remote Sensing Technology Institute
S. Wójtewicz, Nicolaus Copernicus University in Torun
S. N. Yurchenko, University College London
N. F. Zobov, Institute of Applied Physics of Russian Academy of Sciences, Nizhny Novgorod, Russia

Document Type

Article

Publication Date

2026

DOI

10.1016/j.jqsrt.2026.109807

Publication Title

Journal of Quantitative Spectroscopy and Radiative Transfer

Volume

353

Pages

109807

Abstract

The HITRAN database is a curated compilation of validated molecular spectroscopic parameters, established in the early 1970s. It is used by various computer codes to predict and simulate the transmission and emission of light in gaseous media (with an emphasis on terrestrial and planetary atmospheres). The HITRAN compilation is composed of six major components. These components include the line-by-line spectroscopic parameters required for high-resolution radiative-transfer codes, experimentally derived absorption cross-sections (for molecules where it is not yet feasible for representation in a line-by-line form), collision-induced absorption data, aerosol indices of refraction, and general tables (including partition sums) that apply globally to the data. Responding to community requests, HITRAN2024 also incorporates — for the first time — a water-vapor continuum model.

This paper describes the details of the choices of data and their compilation for the 2024 quadrennial edition of HITRAN. The HITRAN2024 edition takes advantage of recent experimental and theoretical data that were meticulously validated, in particular, against laboratory and atmospheric spectra. The new edition replaces the previous HITRAN edition of 2020 (including various updates during the intervening years).

The extent of the updates of the line-by-line section in the HITRAN2024 edition ranges from updating a few lines of specific molecules/isotopologues to complete replacements of the lists, and also the introduction of additional isotopologues and six new (to HITRAN) molecules: H₃+, CH₃, S₂, COFCl, HONO, ClNO₂. Many new vibrational bands were added, extending the spectral coverage and completeness of the line lists. In addition, the accuracy of the parameters for major atmospheric absorbers has been increased substantially, often bringing the uncertainties down to unprecedented levels below 0.1%.

The HITRAN2024 edition is available through www.hitran.org as well as the HITRAN Application Programming Interface (HAPI). The functionality of the tools to work with the HITRAN data has been extended for the new edition.

Rights

© 2026 Battelle Memorial Institute.

This is an open access article under the Creative Commons Attribution 4.0 International (CC BY 4.0) License.

Data Availability

Article states: "This article describes public database."

Original Publication Citation

Gordon, I. E., Rothman, L. S., Hargreaves, R. J., Gomez, F. M., Bertin, T., Hill, C., Kochanov, R. V., Tan, Y., Wcisło, P., Makhnev, V. Y., Bernath, P. F., Birk, M., Boudon, V., Campargue, A., Coustenis, A., Drouin, B. J., Gamache, R. R., Hodges, J. T., Jacquemart, D.,…Zobov, N. F. (2026). The HITRAN2024 molecular spectroscopic database. Journal of Quantitative Spectroscopy and Radiative Transfer, 353, Article 109807. https://doi.org/10.1016/j.jqsrt.2026.109807

ORCID

0000-0002-1255-396X (Bernath)

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