1.3 MM emission in the disk of NGC 891: Evidence of cold dust

Details 1.3 MM emission in the disk of NGC 891: Evidence of cold dust 1.3 MM emission in the disk of NGC 891: Evidence of cold dust

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...279l..37g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 279, no. 2, p. L37-L40

Astronomy and Astrophysics

Astronomy

82

Cosmic Dust, Interstellar Gas, Interstellar Matter, Molecular Clouds, Molecular Spectra, Radio Astronomy, Radio Spectra, Spiral Galaxies, Astronomical Spectroscopy, Carbon Monoxide, Emission Spectra, Hydrogen, Hydrogen Compounds, Iodides, Line Spectra, Radio Telescopes

Scientific paper

Using the Institut de Radio Astronomie Millimetrique (IRAM) 30-m telescope equipped with the Max-Planck-Institut fuer Radioastronomie (MPIfR) 7-channel bolometer array, we have mapped the lambda-1.3 mm continuum emission of NGC 891, an edge-on Sb galaxy similar to the Milky Way. This emission is 7 times stronger along the major axis than the CO 2-1 line averaged over the 50 GHz bolometer passband, and 9 times stronger than the warm dust emission expected from the IRAS data. The lambda-1.3 mm dust emission correlates remarkably well with the CO emission and poorly with HI emission, at least up to +/- 7 kpc (150 sec) from the center. It arises mostly from cold dust (T less than or = 20 K) associated with molecular clouds. The H2 mass, calcuclated using Galactic values of the dust absorption cross section, is approximately 3 times smaller than the H2 mass derived from the CO luminosity and Strong et al's (1988) 'standard' Galactic CO to H2 conversion factor. It is about equal to the HI mass inside a 7 kpc radius. The mass of gas associated with the cold dust is approximately 20 times the mass of gas associated with warm dust.

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