The kinematics of the molecular gas in Centaurus A

Details The kinematics of the molecular gas in Centaurus A The kinematics of the molecular gas in Centaurus A

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...391..121q&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 391, no. 1, May 20, 1992, p. 121-136. Research supported by Alfred P. Sloan

Astronomy and Astrophysics

Astrophysics

79

Galactic Structure, Gas Dynamics, Interstellar Gas, Molecular Gases, Radio Galaxies, Astronomical Models, Carbon Monoxide, Centaurus Constellation, Emission Spectra

Scientific paper

The CO (2-1) emission along the inner dust lane of Centaurus A, observed with the Caltech Submillimeter Observatory on Mauna Kea, shows the molecular gas to be in a thin disk, with a velocity dispersion of only about 10 km/s. The observed line profiles are broadened considerably due to beam smearing of the gas velocity field. The profile shapes are inconsistent with planar circular and noncircular motion. However, a warped disk in a prolate potential provides a good fit to the profile shapes. The morphology and kinematics of the molecular gas is similar to that of the ionized material, seen in H-alpha. The best-fitting warped disk model not only matches the optical appearance of the dust lane but also agrees with the large-scale map of the CO emission and is consistent with H I measurements at larger radii.

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