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Astron. Astrophys. 325, 923-932


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The extended CO J=1-0 emission in NGC 253

S. Houghton1, J.B. Whiteoak2, B. Koribalski2, R. Booth3, T. Wiklind3, and R. Wielebinski4

1Department of Astrophysics & Optics, School of Physics, University of New South Wales, Sydney NSW 2052, Australia
2Australia Telescope National Facility, PO Box 76, Epping NSW 2121, Australia
3Onsala Space Observatory, S-43992, Onsala, Sweden
4Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

Received 10 January 1997 / Accepted 11 March 1997

Abstract

The distribution of 12CO(1-0) has been mapped over the spiral galaxy NGC 253 using the Swedish-ESO Submillimetre Telescope (SEST). Emission was found to extend 22.4 arcmin along the major axis and to be concentrated towards the nucleus with an LSR systemic velocity of 235 km s-1. The CO intensity and velocity distribution suggests three subsystems: a dense, highly-rotating nuclear cloud, a disk (with a line of nodes at a position angle of 63FORMULA ) extending 150 arcsec each side of the nucleus containing a bar or spiral arms that are located at an azimuth of 21FORMULA , and an outer disk with a position angle of 52FORMULA. The total gas mass derived for the full extent is FORMULA , about 2% of the calculated dynamic mass of FORMULA .

Key words: galaxies: individual: NGC 253 - galaxies: kinematics and dynamics - radio lines: ISM

Send offprint requests to: sjh@wodin.phys.unsw.edu.au


© European Southern Observatory (ESO) 1997

Online publication: September 9, 1997
Last change: April 28, 1998
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