EDP Sciences
Free Access
Volume 394, Number 3, November II 2002
Page(s) 823 - 833
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361:20021232
Published online 21 October 2002

A&A 394, 823-833 (2002)
DOI: 10.1051/0004-6361:20021232

Abundant molecular gas in the intergalactic medium of Stephan's Quintet

U. Lisenfeld1, J. Braine2, P.-A. Duc3, S. Leon1, 4, V. Charmandaris5, 6 and E. Brinks7, 8

1  Instituto de Astrofísica de Andalucía, CSIC, Apdo. 3004, 18080 Granada, Spain
2  Observatoire de Bordeaux, UMR 5804, CNRS/INSU, BP 89, 33270 Floirac, France
3  CNRS URA 2052 and CEA/DSM/DAPNIA Service d'Astrophysique, Saclay, 91191 Gif sur Yvette Cedex, France
4  Physikalisches Institut, University of Cologne, Germany
5  Cornell University, Astronomy Department, Ithaca, NY 14853, USA
6  Chercheur Associé, Observatoire de Paris, LERMA, 75014 Paris, France
7  Departamento de Astronomía, Universidad de Guanajuato, Apdo. Postal 144, Guanajuato, Gto 36000, Mexico
8  INAOE, Apdo. Postal 51 & 216, Puebla, Pue 72000, Mexico

(Received 24 May 2002 / Accepted 23 August 2002 )

Stephan's Quintet (SQ) is a system consisting of at least four interacting galaxies which is well known for its complex dynamical and star formation history. It possesses a rich intergalactic medium (IGM), where hydrogen clouds, both atomic and molecular, associated with two starbursts (refered to as SQ A and B) have been found. In order to study the extent, origin and fate of the intergalactic molecular gas and its relation to the formation of stars outside galaxies and Tidal Dwarf Galaxies (TDGs), we mapped with the IRAM 30 m antenna the carbon monoxide (CO) towards several regions of the IGM in SQ. In both SQ A and B, we detected unusually large amounts of molecular gas ( $3.1 \times 10^9$  $M_\odot$ and $7 \times 10^8$  $M_\odot$, respectively). In contrast, no significant CO detection was achieved towards HII regions south of the pair NGC 7318a/b despite their high H $\alpha$ luminosities. The molecular gas is very extended in both SQ A and SQ B, over areas of between 15 and 25 kpc. The CO clouds seem to have otherwise different properties and may be of a different nature. The integrated CO line of SQ A is in particular much wider than in SQ B. Its CO spectrum shows emission at two velocities (6000 and 6700 km s -1) that are coincident with two HI lines. The strongest emission at 6000 km s -1 is however spatially offset from the HI emission and situated on a ridge south-east of the starburst region. In SQ B the CO emission coincides with that of tracers of star formation (H $\alpha$, 15  $\mu$m and radio continuum). The CO peak lies slightly offset from the HI peak towards a steep HI gradient. This is indicating that the molecular gas is forming in-situ, possibly in a region of compressed HI, with subsequent star formation. The star forming region at SQ B is the object in SQ that most resembles a TDG.

Key words: galaxies: clusters: individual: Stephan's Quintet -- galaxies: individual: NGC 7319, NGC 7318b -- galaxies: interaction -- galaxies: ISM -- intergalactic medium

Offprint request: U. Lisenfeld, ute@iaa.es

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© ESO 2002

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