HITRANonline

There are now over 11000 users registered on www.hitran.org

Dear Colleagues,

The data on this website corresponds to the recently released HITRAN2016 edition of the database. The HITRAN2016 paper describing the new edition is available in Open Access

I.E. Gordon, L.S. Rothman, C. Hill, R.V. Kochanov, Y. Tan, P.F. Bernath, M. Birk, V. Boudon, A. Campargue, K.V. Chance, B.J. Drouin, J.-M. Flaud, R.R. Gamache, J.T. Hodges, D. Jacquemart, V.I. Perevalov, A. Perrin, K.P. Shine, M.-A.H. Smith, J. Tennyson, G.C. Toon, H. Tran, V.G. Tyuterev, A. Barbe, A.G. Császár, V.M. Devi, T. Furtenbacher, J.J. Harrison, J.-M. Hartmann, A. Jolly, T.J. Johnson, T. Karman, I. Kleiner, A.A. Kyuberis, J. Loos, O.M. Lyulin, S.T. Massie, S.N. Mikhailenko, N. Moazzen-Ahmadi, H.S.P. Müller, O.V. Naumenko, A.V. Nikitin, O.L. Polyansky, M. Rey, M. Rotger, S.W. Sharpe, K. Sung, E. Starikova, S.A. Tashkun, J. Vander Auwera, G. Wagner, J. Wilzewski, P. Wcisło, S. Yu, E.J. Zak, The HITRAN2016 Molecular Spectroscopic Database, J. Quant. Spectrosc. Radiat. Transf. (2017) 203, 3-69.
doi:10.1016/j.jqsrt.2017.06.038.]

==> Note that we are still making ongoing improvements to many molecular bands. Updates, improvements, and corrections to the edition are posted in the "Database Updates" panel located on the home page of the HITRAN web-site. When citing the database it is recommended to indicate if an updated version of the HITRAN2016 edition was used.

Please e-mail to us (info@hitran.org) a summary of any serious problems you encounter (or successes or suggestions).

  Three articles that are very helpful in assisting users in learning how to work with new tools and parameters in the HITRAN database have recently been published in JQSRT.

1. Article describing structure and working capabilities of HITRANonline (www.hitran.org):
Hill, C., Gordon, I. E., Kochanov, R. V., Barrett, L., Wilzewski, J. S., Rothman, L. S. (2016). HITRANonline: An online interface and the flexible representation of spectroscopic data in the HITRAN database. JQSRT, 177, 4–14. http://doi.org/10.1016/j.jqsrt.2015.12.012

2. Article describing working capabilities of HITRAN Application Programming Interface (HAPI) (www.hitran.org/hapi):
Kochanov, R. V., Gordon, I. E., Rothman, L. S., Wcisło, P., Hill, C., Wilzewski, J. S. (2016). HITRAN Application Programming Interface (HAPI): A comprehensive approach to working with spectroscopic data. JQSRT, 177, 15–30. http://doi.org/10.1016/j.jqsrt.2016.03.005

3. Article describing implementation of the Hartmann-Tran profile in the HITRAN database:
Wcisło, P., Gordon, I. E., Tran, H., Tan, Y., Hu, S.-M., Campargue, A., Romanini, D., Hill, C., Kochanov, R.V., Rothman, L. S. (2016). The implementation of non-Voigt line profiles in the HITRAN database: H2 case study. JQSRT, 177, 75–91. http://doi.org/10.1016/j.jqsrt.2016.01.024

The HITRAN support e-mail has been established and our team is ready for questions.

The NO line list has undergone a substantial update for all three isotopologues (¹⁴N¹⁶O, ¹⁵N¹⁶O, ¹⁴N¹⁸O). For ¹⁴N¹⁶O, the new wavenumber range covers 0-23,730 cm^-1 and includes bands with a maximum Δv=14 for the X ²Π electronic ground state. For ¹⁵N¹⁶O and ¹⁴N¹⁸O, the coverage is now up to 15,650 cm^-1. The primary source of the update has been the semi-empirical work of Wong et al. (2017), MNRAS 470, 882, however new hyperfine split line parameters have also been updated from Müller et al. (2015), JMS 310, 92. Also, ab initio intensities of some of the bands have been scaled to match experimental values.

In addition, the available data for air- and self-broadening parameters have been refit to a function that performs better for high J. The pressure shifts have also been updated to extend the measurements of Spencer et al. (1994), JMS 165, 506 to higher Δv.

The format for the wavenumber parameter has been adapted to enable an increased precision for the MW transitions, as has been previously done for HNO₃, PH₃, O₂ and NO⁺.

The line-mixing package for CO₂ had been updated, to make input line-widths consistent with the actual widths provided to the database, with an exception to when these line-widths were obtained with speed-dependent Voigt profile rather than Voigt. In that case alternative approach was used. In some regions the change results in appreciable differences corresponding to decrease of the residuals when applied to real laboratory data. The line-mixing package is available at http://hitran.org/suppl/LM/

Parameters associated with broadening of spectral lines by the pressure of ambient water vapor have been added to the database for the first time. In this first installment we added broadening parameter gamma_H2O to all lines of carbon dioxide (CO₂).

It was discovered that the Einstein-A coefficients for all transitions of both isotopologue of phosgene were calculated erroneously in HITRAN2016. These parameters have been corrected in this update.

It was discovered that about 1500 lines with intensities of the order of 10^-28 cm/molecule in the 8340-10240 cm^-1 region were accidentally omitted from the database. These lines have been restored from the HITRAN 2012 edition. Also a small number of lines were removed or reassigned, fixing errors associated with different assignments of lines in the linelists that were combined together to form the HITRAN2016 edition.

Note that a very substantial update is underway to correct a number of errors associated with erroneous calculations of the statistical weights for some of the isotopologues of water vapor, especially D₂. The upcoming update however will not largely affect line positions nor intensities for most of the water vapor lines in HITRAN.

The broadening parameters of CO lines due to the pressure of CO₂, and especially their temperature dependencies, were updated using data from Hashemi et al, J of Molec Spectrosc (2016) 326, 60-72.

It was found that due to a programming error 19 lines (with P1_e assignment) of some bands of asymmetric isotopologues of carbon dioxide had air-broadened half-width values of zero in the official release of HITRAN2016. This has been fixed now and all of these lines have appropriate values for this parameter.

In addition the pure rotational transitions of the ¹⁶O¹²C¹⁷O isotopologue were missing upper-state quantum numbers associated with the hyperfine splitting. This in turn caused erroneous calculation of the upper-state statistical weight and the Einstein-A coefficients. All of these weak lines have been fixed now.

Once again we would like to remind users that the 11^th and 12^th isotopologues of carbon dioxide are labeled as A and B respectively if one asks for the output in the ".par" format. This should be taken into account in radiative transfer codes.