# ABSOLUTE INTENSITIES OF $O_{3}$ LINES IN THE $9-11 \mu$m REGION

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/19136

Files Size Format View
1998-WF-04.jpg 210.9Kb JPEG image

 Title: ABSOLUTE INTENSITIES OF $O_{3}$ LINES IN THE $9-11 \mu$m REGION Creators: Smith, M. A. H.; Rinsland, C. P.; Devi, V. Malathy; Benner, D. Chris Issue Date: 1998 Publisher: Ohio State University Abstract: We have completed our analysis of high-resolution $(0.0027 cm^{-1})$ absorption spectra of $ozone^{a}$ to determine absolute intensities of $376 ^{16}O_{3}$ lines in the $9-11 \mu$m region. The spectra were recorded at room temperature using the Fourier transform spectrometer at the McMath-Pierce facility of the National Solar Observatory at Kitt Peak. The ozone samples were contained in a glass cell having crossed IR-transmitting and UV-transmitting paths approximately 10 cm in each direction. The ozone partial pressures (0.3 to 0.5 Torr) in the cell were determined from measurements of the 254 nm UV-absorption, using the absorption cross-section of Maucrsberger $et al.^{b}$ as a reference standard. Only spectra for which the ozone partial pressure varied by $< 1.0$\% during the recording time were selected for analysis. A multispectrum nonlinear least-squares $procedure^{c}$ was used to fit four spectra simultaneously to determine intensities for 366 lines in the P, Q, and R branches of the $\nu_{3}$ fundamental band and 10 lines in the R branch of the $\nu_{1}$ band. The absolute accuracy of these intensity values ranges from 2\% for the strongest, most well-determined lines to 4 or 5\% for the weakest lines measured. On average, our measured intensities are approximately 1\% larger than the values on the current HITRAN $compilation.^{d}$ Our measurement set includes $44 \nu_{3}$ lines in common with other recent experimental $studies,^{e f g}$ Comparison of these various measurements shows excellent agreement for a few lines and adequate agreement (considering all possible sources of uncertainty and systematic errors) for the others. Description: $^{a}$ M.A.H. Smith, C.P. Rinsland, V. Malathy Devi, and D. Chris Benner, 52nd International Symposium on Molecular Spectroscopy, Paper RF03 (1997). $^{b}$ K. Mauersberger, D. Hanson, J. Barnes, and J. Morton, J. Geophys. Res. 92, 8480-8482 (1987) $^{c}$ D. Chris Benner, C.P. Rinsland, V. Malathy Devi, M.A.H. Smith, and D. Atkins, JQSRT 53. 705-721 (1995). $^{d}$ L.S. Rothman et al., JQSRT 48, 469-507 (1992); L.S. Rothman et al., JQSRT, in press (1998). $^{e}$ H.M. Pickett, D.B. Peterson, and J.S. Margolis, J. Geophys. Res. 97, 20,787-20,793 (1992). $^{f}$ M.R. DeBacker, B. Parvitte, V. Zeninari, and D. Courtois, JQSRT 54, 1009-1018 (1995). $^{g}$ M.R. DeBacker-Barilly and D. Courtois, Appl. Phys. B 64, 607-611 (1997). Author Institution: Atmospheric Sciences Division, NASA Langley Research Center; Department of Physics, The College of William and Mary URI: http://hdl.handle.net/1811/19136 Other Identifiers: 1998-WF-04