Issue |
A&A
Volume 415, Number 1, February III 2004
|
|
---|---|---|
Page(s) | L1 - L5 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361:20031744 | |
Published online | 03 February 2004 |
Letter to the Editor
Mapping the cold molecular gas in a cooling flow cluster: Abell 1795
LERMA, Observatoire de Paris, 61, Av. de l'Observatoire, 75014 Paris, France
Corresponding author: P. Salomé, philippe.salome@bspm.fr
Received:
31
October
2003
Accepted:
16
December
2003
Cold molecular gas is found in several clusters of galaxies
(Edge [CITE]; Salomé & Combes [CITE]): single dish telescope observations in
CO(1–0) and CO(2–1) emission lines have revealed the existence of
large amounts of cold gas (up to ~1011 ) in the
central region of cooling flow clusters. We present here
interferometric observations performed with the IRAM Plateau de Bure
interferometer in Abell 1795. Comparison with IRAM 30 m data shows the
cold gas detected is extended suggesting a cooling flow origin.
The CO features identified are very similar to the
structures observed in Hα and with the star forming regions observed
through UV continuum excess. A large fraction of the cold gas is not
centered on the central cD, but located near
brightest X-ray emitting regions along the North–West orientated radio
lobe. The cold gas kinematics is consistent with the optical
nebulosity behaviour in the very central
region. It is not in rotation
around the central cD: a velocity gradient shows the cold gas
might be cooled gas from the intra-cluster medium being accreted by the central galaxy.
The optical filaments, aligned with the cD orbit, are intimately related to the
radio jets and lobes. The material fueling the star formation
certainly comes from the deposited gas, cooling more
efficiently along the edge of the radio lobes. Even
if some heating mechanisms are present, these millimetric observations show
that an effective cooling to very low temperatures indeed occurs and is probably
accelerated by the presence of the radio source.
Key words: galaxies: clusters: individual: Abell 1795 / cooling flows / molecular gas
© ESO, 2004
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