The physical state of the obscuring torus in Seyfert galaxies

Details The physical state of the obscuring torus in Seyfert galaxies The physical state of the obscuring torus in Seyfert galaxies

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..179k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 1, 1989, p. 179-185.

Statistics

Computation

95

Computational Astrophysics, Galactic Nuclei, Molecular Clouds, Seyfert Galaxies, Abundance, Carbon Monoxide, Emission Spectra, Near Infrared Radiation, Toruses

Scientific paper

Calculations are presented describing the ionization, chemical, and thermal state of molecular material in the obscuring tori close to the nuclei of many Seyfert galaxies. These are unusual molecular clouds: their electron fractions are about .001 and their temperatures are about 1000 K. Cooling is accomplished primarily by radiation of NIR H2 lines and FIR CO lines. High-J (C-12)(O-16) rotational lines should eventually be detectable from the nearer Seyfert galaxies. Medium-J lines due to (C-13)(O-16) and (C-12)(O-18) as well as (C-12)(O-16) should also be strong. Because ordinary molecular clouds are weak in these lines, the nuclear CO emissions can be distinguished from CO emission farther out in the host galaxy's disk.

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