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The kinematics of the molecular gas in Centaurus AThe 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.
Document ID
19920055085
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Quillen, A. C.
(NASA Headquarters Washington, DC United States)
De Zeeuw, P. T.
(NASA Headquarters Washington, DC United States)
Phinney, E. S.
(NASA Headquarters Washington, DC United States)
Phillips, T. G.
(California Institute of Technology Pasadena, United States)
Date Acquired
August 15, 2013
Publication Date
May 20, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 391
Issue: 1 Ma
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A37709
Funding Number(s)
CONTRACT_GRANT: NSF AST-88-15132
CONTRACT_GRANT: NAGW-2144
CONTRACT_GRANT: NAGW-2142
Distribution Limits
Public
Copyright
Other

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