Journal of Quantitative Spectroscopy and Radiative Transfer
The GEISA data bank in 1993: A PC/AT compatible computers' new version
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Cited by (36)
TheoReTS – An information system for theoretical spectra based on variational predictions from molecular potential energy and dipole moment surfaces
2016, Journal of Molecular SpectroscopyCitation Excerpt :Most of the corresponding line lists are essentially compilations of observed data or include calculated parameters fitted to laboratory experimental measurements using effective spectroscopic models. The success of these efforts for remote sensing, climate modeling and environmental applications has conducted to a diversification of the concepts of spectroscopic information systems, many of them being also accompanied by software tool and graphical interface for spectral functions simulation [15,16,5,17–19] and see also the links to GEISA (http://www.pole-ether.fr/geisa/), HITRAN on the web (http://hitran.iao.ru/) and HAPI (http://hitran.org/static/hapi/hapi_manual.pdf). New fields of applications have recently emerged due to astronomical observations using space-based and ground-based telescopes.
The 2003 edition of the GEISA/IASI spectroscopic database
2005, Journal of Quantitative Spectroscopy and Radiative TransferCitation Excerpt :Consequently, a strong demand exists for a highly comprehensive, well-validated, efficiently operational, and desirably interactive computer-based spectroscopic database. In order to meet demands such as these, the ARA group at LMD (see [1–4]) has been engaged during the past three decades in the development of GEISA. It is a computer-accessible database and was designed to facilitate accurate and fast, forward calculations of atmospheric radiative transfer using a line-by-line and (atmospheric) layer-by-layer approach.
The far-infrared spectra of Jupiter and Saturn
2004, Planetary and Space ScienceCitation Excerpt :Our vertical profile for the mixing ratio of PH3 in Saturn differs from the one determined by Davis et al. (1996). That analysis used PH3 line intensities from the 1992 GEISA compilation (Husson et al., 1994) which were later found to be incorrect. The lines from methane were barely detectable in our spectra of Saturn, hence a reliable estimate of the CH4 abundance on this planet was not possible.
A new software tool for radiative transfer calculations and its application to IMG/ADEOS data
2001, Journal of Quantitative Spectroscopy and Radiative Transfer