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dc.contributor.authorLisenfeld, U.
dc.contributor.authorBraine, J.
dc.contributor.authorDuc, P.A.
dc.contributor.authorLeon, S.
dc.contributor.authorCharmandaris, V.
dc.contributor.authorBrinks, E.
dc.date.accessioned2007-08-11T20:14:10Z
dc.date.available2007-08-11T20:14:10Z
dc.date.issued2002-11
dc.identifier.citationLisenfeld , U , Braine , J , Duc , P A , Leon , S , Charmandaris , V & Brinks , E 2002 , ' Abundant molecular gas in the intergalactic medium of Stephan's Quintet ' , Astronomy and Astrophysics , vol. 394 , pp. 823-833 . https://doi.org/10.1051/0004-6361:20021232
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 174163
dc.identifier.otherPURE UUID: 63107159-10b8-45fa-b541-f8b1be424ca0
dc.identifier.otherdspace: 2299/345
dc.identifier.otherScopus: 0036847057
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407878
dc.identifier.urihttp://hdl.handle.net/2299/345
dc.descriptionOriginal article can be found at http://www.aanda.org/ Copyright The European Southern Observatory DOI : 10.1051/0004-6361:20021232
dc.description.abstractStephan'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 IRAM30 m antenna the carbon monoxide (CO) towards several regions of the IGMin SQ. In both SQ A and B, we detected unusually large amounts of molecular gas (3:1 109 M and 7 108 M , respectively). In contrast, no significant CO detection was achieved towards HII regions south of the pair NGC 7318a/b despite their high H 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 , 15 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.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
dc.titleAbundant molecular gas in the intergalactic medium of Stephan's Quinteten
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2002-11
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361:20021232
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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