Far-Infrared [C II] Emission from the Central Regions of Spiral Galaxies

Details Far-Infrared [C II] Emission from the Central Regions of Spiral Galaxies Far-Infrared [C II] Emission from the Central Regions of Spiral Galaxies

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jkas...37..193m&link_type=abstract

Journal of the Korean Astronomical Society, vol. 37, no. 4, pp. 193-197

Astronomy and Astrophysics

Astronomy

1

Galaxies: Individual (Milky Way, M31), Galaxies: Ism, Galaxies: Spiral, Infrared: Ism, Ism: Lines And Bands

Scientific paper

Anomalies in the far-infrared [C II] 158 μm line emission observed in the central one-kiloparsec regions of spiral galaxies are reviewed. Low far-infrared intensity ratios of the [C II] line to the continuum were observed in the center of the Milky Way, because the heating ratio of the gas to the dust is reduced by the soft interstellar radiation field due to late-type stars in the Galactic bulge. In contrast, such low line-to-continuum ratios were not obtained in the center of the nearby spiral M31, in spite of its bright bulge. A comparison with numerical simulations showed that a typical column density of the neutral interstellar medium between illuminating sources at hν ˜ 1 eV is NH ≲ 1021 cm-2 in the region; the medium is translucent for photons sufficiently energetic to heat the grains but not sufficiently energetic to heat the gas. This interpretation is consistent with the combination of the extremely high [C II]/CO J = 1--0 line intensity ratios and the low recent star-forming activity in the region; the neutral interstellar medium is not sufficiently opaque to protect the species even against the moderately intense incident UV radiation. The above results were unexpected from classical views of the [C II] emission, which was generally considered to trace intense interstellar UV radiation enhanced by active star formation.

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