Issue |
A&A
Volume 373, Number 3, July III 2001
|
|
---|---|---|
Page(s) | 853 - 880 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20010670 | |
Published online | 15 July 2001 |
Warm gas in central regions of nearby galaxies
Extended mapping of CO(3-2) emission
1
SMTO, Steward Observatory, The University of Arizona, 933 N. Cherry Avenue, Tucson, Arizona 85721, USA
2
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
3
Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, 38406 St. Martin d'Hères, France
Corresponding author: M. Dumke, mdumke@as.arizona.edu
Received:
30
August
2000
Accepted:
3
May
2001
We have mapped the CO(3-2) line emission from several nearby galaxies,
using the Heinrich-Hertz-Telescope on Mt. Graham, Arizona. Unlike earlier
observations, our investigation is not restricted to starburst galaxies,
but includes twelve galaxies of various types and in different stages of
star forming activity. Furthermore, we have not only observed the central
positions of these objects, but have obtained maps of the extended
CO(3-2) emission, with a typical map extent of 2 to 3 arcmin in each
direction. Our
observations show that this extended mapping is necessary to reveal spatial
changes of the ISM properties within the galaxies.
In this paper we present the data sets and some data analysis. We compare
the galaxies in view of their morphology and excitation conditions, using
line ratios, luminosities and other properties, like the extent of the
CO(3-2) emission. The main results of this CO(3-2) survey are:
1. In none of the observed objects the emission is confined to the nucleus,
as claimed in some earlier publications. CO(3-2) emission can be detected
for some objects to the same extent as the CO(2-1) and the CO(1-0) lines.
2. The emission is more concentrated to the vicinity of star forming
structures (nuclear regions and spiral arms) than the lower CO transitions
for most of the observed objects. This is shown by decreasing
(3-2)/(1-0) line intensity ratios from the very centres towards larger
radii. The (deconvolved) sizes of the central emission peaks in the
CO(3-2) line vary from about 300 pc up to 3 kpc.
3. The CO(3-2) luminosity is stronger in objects that contain
a nuclear starburst or morphological peculiarities. The total power emitted
in the CO(3-2) line from the central regions (i.e. excluding spiral
arms/outer disk) is highest in the starburst galaxies NGC 2146, M 82,
NGC 3628, and in the spiral galaxy M 51. When comparing the total power
normalized to the size of the emission region, the starburst galaxies
M 82 and NGC 253 show the highest values (about three times higher
than most other objects), while NGC 278 and NGC 4631 show the lowest.
4. With the present spatial resolution, the line ratios seem to
be independent of Hubble type, color or luminosity. Most galaxies with
enhanced central star formation ("starbursts" ) show line ratios
of the integrated intensities of
in the very centre and ~1.0 at a radius
of about 1 kpc. Objects with a ring-like (or double-peak if seen
edge-on) molecular gas distribution (NGC 253, M 82, and NGC 4631)
show lower ratios.
The two galaxies that have CO(3-2) emission distributed over their spiral
arms (NGC 891 and M 51) show very low line ratios despite their high
infrared luminosities. This result suggests that CO emission in these
objects reflects a large amount of molecular gas, but not enhanced star
forming activity.
5. Starburst galaxies show CO(3-2) emission also in their disks.
The line intensities are higher than that of normal galaxies. This suggests
that even if a starburst is a localized phenomenon, it is related to
different properties of the molecular gas over the whole galaxy.
Key words: galaxies: ISM / galaxies: spiral / radio lines: galaxies
© ESO, 2001
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