CO to H2 Ratio of Diffuse Interstellar Molecular Clouds

Details CO to H2 Ratio of Diffuse Interstellar Molecular Clouds CO to H2 Ratio of Diffuse Interstellar Molecular Clouds

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.9902l&link_type=abstract

American Astronomical Society Meeting 204, #99.02; Bulletin of the American Astronomical Society, Vol. 36, p.985

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Scientific paper

We present measurements of interstellar H2 and CO absorption lines in the continuum spectra of 7 early-type stars that were observed with the Berkeley Extreme and Far-ultraviolet Spectrometer (BEFS) on the ORFEUS telescope and the Far Ultraviolet Spectroscopic Explorer (FUSE). Although the BEFS has a moderate resolving power of 3000 at FUV wavelengths (912-1170 Å), it is suited for analyzing H2 absorption lines of bright FUV sources. From the 54 early-type target stars in the Galactic disk and halo observed by the BEFS, we choose our 7 program stars (HD 37903, HD 97991, HD 149881, HD 156110, HD 164794, HD 214080 and HD 219188), which have only a single velocity component in the high-resolution optical measurements, to avoid line blending. The H2 column density of the 7 interstellar molecular clouds ranges from 3.5 x 1017 to 7.9 x 1020 cm-2, and the kinetic temperature T01 ranges from 36 to 211 K. To analyze the CO molecule, we select the E-X (0-0) band at 1076 Å, which has a large oscillator strength and is not blended with other interstellar absorption lines. We detect the CO absorption line in 3 (HD 37903, HD 164794, and HD 214080) of the 7 FUSE spectra and derive CO column densities for those targets. Since the amount of CO in the interstellar molecular clouds is a function not only of the H2 column but also of the physical conditions of the cloud, e.g. temperature, density, and UV intensity, we investigate the CO column densities according to those physical conditions derived from the H2 analysis.

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