[CII] 158 micron absorption line towards the Galactic Center: connection with bright IR galaxies

Details [CII] 158 micron absorption line towards the Galactic Center: connection with bright IR galaxies [CII] 158 micron absorption line towards the Galactic Center: connection with bright IR galaxies

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.511..225v&link_type=abstract

Exploiting the ISO Data Archive. Infrared Astronomy in the Internet Age, held in Siguenza, Spain 24-27 June, 2002. Edited by

Astronomy and Astrophysics

Astronomy

Scientific paper

Located near the galactic center, Sgr B2 is one of the largest HII/molecular cloud complexes in the Galaxy. The total mass and compactness of Sgr B2 are comparable to those of the W49N star-forming complex (Vastel et al. 2000, Vastel et al. 2001). We present high spectral resolution Fabry-Pérot observations of the [OI] 63.2 and 145.5 μm and [CII] 157.7 μm fine structure lines obtained with ISO-LWS. Observations of the CO isotopes and the HI lines reveal that three different layers containing atomic oxygen can be disentangled as predicted by PDRs models. These layers are characterized by different forms of carbon in the gas phase, i.e. the C+ external layer, the C+ to C0 transition and the CO internal layer. We derive lower limits for the column densities of atomic carbon and oxygen of the order of ˜ 1018 cm-2 and 3 × 1019 cm-2, respectively. An O0/CO ratio of around 2.5 is computed in the internal cores of the clouds lying along the line of sight, which means that ˜ 70% of gaseous oxygen is in the atomic form and not locked into CO. The fact that the [CII] 157.7 μm line is detected in absorption implies that the main cooling line of the interstellar medium can be optically thick especially in the direction of large star-forming complexes or in the nuclei of galaxies. This could partially account for the deficiency in the [CII] 157.7 μm line which has been recently found toward infrared bright galaxies in ISO data.

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