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5.12. High-resolution CO (1-0) observations of the ringed galaxy NGC 4736

Published online by Cambridge University Press:  25 May 2016

Tony Wong ,
Tamara Helfer  and
Leo Blitz
Tony Wong
Affiliation:
University of California at Berkeley, Berkeley, CA 94720 U.S.A. e-mail: twong@astro.berkeley.edu
Tamara Helfer
Affiliation:
University of California at Berkeley, Berkeley, CA 94720 U.S.A. e-mail: twong@astro.berkeley.edu
Leo Blitz
Affiliation:
University of California at Berkeley, Berkeley, CA 94720 U.S.A. e-mail: twong@astro.berkeley.edu

Extract

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It is well known that the radial distributions of atomic and molecular gas differ markedly in spiral galaxies, including our own (e.g. Burton & Gordon 1978, Sofue et al. 1995). We have recently begun a program to obtain multifrequency observations of several nearby galaxies in order to determine whether H I is needed to replenish the H2 consumed by star formation and, if so, how this might be accomplished. Here we present initial results on the nearby RSab galaxy NGC 4736, known for its bright ring of H II regions and recently shown to have a central stellar bar (Möllenhoff et al. 1995). We have mapped the distribution of CO (1-0) emission within r=1′ (1.8 kpc at D=6.2 Mpc) with the BIMA interferometer at ~5″ resolution, and added data from the NRAO 12-m telescope to recover zero-spacing information.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 235 - 236
Copyright
Copyright © Kluwer 1998 

References

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