Line Intensities and Self-broadening Coefficients of Carbon Dioxide from 4600 to 7000 cm-1

Details Line Intensities and Self-broadening Coefficients of Carbon Dioxide from 4600 to 7000 cm-1 Line Intensities and Self-broadening Coefficients of Carbon Dioxide from 4600 to 7000 cm-1

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6211t&link_type=abstract

American Astronomical Society, DPS meeting #38, #62.11; Bulletin of the American Astronomical Society, Vol. 38, p.607

Astronomy and Astrophysics

Astronomy

Scientific paper

Line positions and strengths are measured for 58 vibrational bands between 4550 and 7000 cm-1. These are retrieved from 42 laboratory spectra recorded using the McMath-Pierce FTIR spectrometer located at Kitt Peak, Arizona. The spectra were recorded using spectral resolutions between 0.01 and 0.013 cm-1. Band strengths in natural abundance range from 3.30x10-20 to 2.8x10-25 cm-1/(molecule cm-2) at 296 K. Comparisons with corresponding values from the literature indicate that absolute accuracies better than 1% and precisions of 0.5% are achieved for the strongest bands.
Self-broadened widths (HWHM) are reported in natural abundance for 15 bands, and self-induced pressure shift coefficients are obtained for 13 of these bands. The experimental width and pressure shift coefficients are well modeled using empirical expressions. The modeled width coefficients agree with the measured values with standard deviations of less than 1%, while the standard deviations of the fits for the pressure-induced shift coefficients range between 2.3 and 6.7%. Small vibrational and rotational variations are observed in the width coefficients. As expected, pressure-induced shift coefficients vary as a function of the band center frequency, with weaker dependences found in the different bands as a function of the rotational quantum J.
Part of the research described in this paper was performed at the Jet Propulsion laboratory, California Institute of Technology under contracts and cooperative agreements with the National Aeronautics and Space Administration. This material is also based upon work supported by the National Science Foundation under Grant No. ATM-0338475.

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