Absolute Intensities of the OH Meinel bands in the Nightglow

Details Absolute Intensities of the OH Meinel bands in the Nightglow Absolute Intensities of the OH Meinel bands in the Nightglow

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsa41a1041c&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SA41A-1041

Astronomy and Astrophysics

Astrophysics

0310 Airglow And Aurora

Scientific paper

Flux-calibrated high resolution spectra of the night sky have been accumulated for the spectral region of 314 - 1054 nm. The spectra are obtained from two sources: (a) the ESI spectrograph on the Keck II telescope at Mauna Kea with a spectral resolution of 6000 and a temporal resolution of 3000 seconds and (b) coadded spectra (1) from the UVES spectrograph on the VLT (Kueyen) telescope at Cerro Paranal with a spectral resolution of 50000. Emission from the OH X2Π (v'=3-9) Meinel bands are prominent in the spectra allowing absolute intensities to be measured for discrete rotational lines in the main rotational branches for 16 vibrational bands in the ESI spectra (Δ v = -6 to -3) and 20 vibrational bands in the UVES spectrum (Δ v = -7 to -3). Comparison of the band intensities to the earlier photographic measurements of Krassovsky et al.(2) show a systematic deviation with wavelength similar to that deduced by Adler-Golden(3). Several emission bands are observed from most upper state vibrational levels. Comparisons of the band intensity ratios and the rotational branch intensity ratios for these bands show systematic deviations from those calculated using the existing sets of emission coefficients. Progress will be reported on the re-evaluation of the dipole moment function (4) using the present absolute intensities to obtain an improved set of OH emission coefficients. This work was partially supported by NSF grant ATM-0139344. (1) R. W. Hanuschik, Astron. Astrophys. 112, 1157 (2003). (2) V. I. Krassovsky et al., Planet. Space Sci. 9, 883 (1962). (3) S. Adler-Golden, J. Geophys. Res. 102, 19969 (1997). (4) D. D. Nelson et al., J. Chem. Phys. 93, 7003 (1990).

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