Issue |
A&A
Volume 453, Number 2, July II 2006
|
|
---|---|---|
Page(s) | 459 - 475 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20035672 | |
Published online | 16 June 2006 |
Molecular gas in the Andromeda galaxy
1
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: c.nieten@zeiss.de;NNeininger@kpmg.com
2
Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
3
Institut de Radioastronomie Millimétrique, 300 rue de la piscine, 38406 St. Martin d' Hères, France e-mail: guelin@iram.fr
4
Instituto de Radioastronomía Milimétrica, Avenida Divina Pastora 7, 18012 Granada, Spain
Received:
13
November
2003
Accepted:
5
December
2005
Aims.We study the distribution of the molecular gas in the
Andromeda galaxy (M 31) and compare this with the distributions of the
atomic gas and the emission from cold dust at m.
Methods.We obtained a new (J = 1-0)-line
survey of the Andromeda galaxy with the highest resolution to date
(
, or 85 pc along the major axis), observed On-the-Fly
with the IRAM 30-m telescope. We fully sampled an area of
with a velocity resolution of
. In several selected
regions we also observed the
(2-1)-line.
Results.Emission from the (1-0) line was
detected from galactocentric radius
kpc to
kpc with a
maximum in intensity at
kpc. The molecular gas traced by the
(velocity-integrated) (1-0)-line intensity is concentrated in narrow
arm-like filaments, which often coincide with the dark dust lanes
visible at optical wavelengths. Between
kpc and
kpc
the brightest CO filaments define a two-armed spiral pattern that is
described well by two logarithmic spirals with a pitch angle of
7°–8°. The arm-interarm brightness ratio averaged over a
length of 15 kpc along the western arms reaches about 20 compared to 4
for
at an angular resolution of
.
For a constant conversion factor
, the molecular
fraction of the neutral gas is enhanced in the spiral arms and
decreases radially from 0.6 on the inner arms to 0.3 on the arms at
kpc. The apparent gas-to-dust ratios
and
increase by a factor of ~20 between the centre and
, whereas the ratio
only increases by
a factor of 4.
Conclusions.Either the atomic and total gas-to-dust ratios
increase by a factor of ~20 or the dust becomes colder towards
larger radii. A strong variation of with radius seems
unlikely. The observed gradients affect the cross-correlations between
gas and dust. In the radial range
–14 kpc total gas and cold dust
are well correlated; molecular gas correlates better with cold dust
than atomic gas.
The mass of the molecular gas in M 31 within a radius of 18 kpc is
at the adopted
distance of 780 kpc. This is 7% of the total neutral gas mass in M 31.
Key words: ISM: molecules / galaxies: individual: M 31 / galaxies: ISM / galaxies: spiral / radio lines: galaxies
© ESO, 2006
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