Issue |
A&A
Volume 469, Number 1, July I 2007
|
|
---|---|---|
Page(s) | 173 - 187 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20054565 | |
Published online | 05 March 2007 |
Dissipative structures of diffuse molecular gas*
II. The translucent environment of a dense core
1
LRA-LERMA, 24 rue Lhomond, École normale supérieure (Observatoire de Paris), 75231 Paris Cedex 05, France e-mail: hilyblan@iram.fr
2
IRAM, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
Received:
22
November
2006
Accepted:
21
February
2007
Aims. This paper belongs to a series of four, dedicated to the analysis of the dynamical, thermal and chemical properties of translucent molecular gas, with the perspective of characterizing the processes driving the dissipation of supersonic turbulence, an anticipated prerequisite of dense core formation.
Methods.We analyze the small scale morphology and velocity
structure of the parsec-scale environment of a low mass
dense core (1 ). Our work is based on large maps
made with the IRAM-30 m telescope in the two lowest
rotational transitions of 12CO and 13CO with high
angular (20'' or 0.015 pc at 115 GHz) and spectral
(0.055 kms s-1) resolutions. The field is translucent, hence
providing strong constraints on the column density and
physical conditions in the gas.
Results.More than one third of the field mass (6.5 ) lies in
an elongated tail of dense and cold gas, possibly
extending beyond the edge of the map and connected to the
core in space and velocity. This core tail is highly
turbulent and sub-structured into narrow filaments of
aspect ratio up to 20. These are pure velocity structures
with velocity shears in the range 2–10 kms s-1 pc-1. Another
third of the mass, according to the weak extinction of the
field, lies in more dilute molecular and atomic gas. Its
molecular fraction, largely traced by optically thick
12CO lines, is even more turbulent than the dense core
tail. The gas emitting in the broad wings of the 12CO
lines is organized into a conspicuous network of narrow
criss-crossed filaments, whose pattern at the parsec scale
is seen for the first time. The gas there is optically
thin in the 12CO(1–0) line
, warmer
than 25 K and more dilute than 1000 cm-3. These optically
thin 12CO-filaments, though contributing to about 10% of
the mass of the environment, have a CO cooling rate a few
times larger than that of the whole field on
average. Whether dense or dilute, all the filamentary
structures in the field (with transverse sizes
0.015–0.03 pc), are preferentially oriented along the
direction of the magnetic fields, as measured a few
parsecs away. Using the Chandrasekhar-Fermi method, we
estimate the intensity of the magnetic fields intensity in
the dilute molecular gas to be Bpos = 15 μg . We infer
that the turbulent motions in the dilute gas are in the
trans-Alfvénic range.
Conclusions.The 1 dense core is surrounded by a translucent and
highly turbulent environment whose gas dynamics are not
super-Alfvénic. The low mass dense core is not isolated
but still connected to a massive reservoir of dense gas.
Filaments of optically thin 12CO are found to radiate
more efficiently in the CO lines than the whole field on
average. These are the structures that we tentatively
identify with the locus of intermittent dissipation of
turbulence, and for which there is no observational
evidence that they are shocks.
Key words: ISM: kinematics and dynamics / ISM: structure / ISM: magnetic fields / line: profiles
© ESO, 2007
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