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Please use this identifier to cite or link to this item: http://hdl.handle.net/10481/28420

Title: Molecular and ionized gas in the tidal tail in Stephan's Quintet
Authors: Lisenfeld, Ute
Braine, J.
Duc, P.-A.
Brinks, E.
Charmandaris, V.
Leon, S.
Issue Date: 2004
Abstract: We have mapped with the IRAM interferometer at Plateau de Bure (PdBI) the 12CO emission towards intergalactic star forming regions located in the tidal tail stemming from NGC7319, in the Stephan's Quintet compact group of galaxies. The 13CO emission of the same region was observed with the IRAM 30m telescope and optical spectroscopy of several HII regions in the area were obtained with the Calar Alto 3.5m telescope. We recovered with the interferometer about 50% of the CO(1-0) total emission that had been earlier measured with single dish observations. We find two main areas of CO emission: (i) an elongated region towards the area known as SQ B where a Tidal Dwarf Galaxy could currently be forming (ii) a barely resolved area at the tip of the optical tidal arm. Both regions follow dust lanes visible on HST images and their CO peak coincides spatially exactly with the maximum of the Halpha line emission. In SQ B, there is furthermore very good kinematical agreement between the CO, Halpha and HI components. We conclude from these coincidences that the gaseous matter found in quantities in the area is physically associated to the optical tidal tail and thus that the intergalactic atomic hydrogen there was expelled from NGC7319. Furthermore, the relatively high oxygen abundances (about solar) estimated from the optical spectra of the HII regions imply that the gas feeding the star formation originated from the inner regions of the parent galaxy. In SQ B, we derive from different tracers a star formation rate of 0.5 \msun/yr. The inferred molecular gas consumption time of 0.5 Gyr lies in the range of values found for spiral and starburst galaxies. On the other hand, the ratio of 12CO/13CO>25 is much higher than the values found in disks of spiral galaxies. A relatively low opacity for the 12CO gas is the most likely reason.
Sponsorship: U.L. and S.L. are supported by the Spanish MCyT Grant AYA 2002-03338 and by the Junta de Andalucía. V.C. would like to acknowledge the partial support of NASA through contract number 1257184 issued by JPL/Caltech and E.B. acknowledges financial support from CONACyT via project 27607-E.
Publisher: European Southern Observatory (ESO); Springer Verlag
Keywords: Galaxies
Star formation
ISM
Molecules
Clusters
Stephan's Quintet
Interactions
Intergalactic medium
URI: http://hdl.handle.net/10481/28420
ISSN: 0004-6361
1432-0746
Rights : Creative Commons Attribution-NonCommercial-NoDerivs 3.0 License
Citation: Lisenfeld, U.; et al. Molecular and ionized gas in the tidal tail in Stephan's Quintet. Astronomy and Astrophysics, 426(2): 471-479 (2004). [http://hdl.handle.net/10481/28420]
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