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dc.contributor.authorBoquien, M.
dc.contributor.authorDuc, P.A.
dc.contributor.authorWu, Y.
dc.contributor.authorCharmandaris, V.
dc.contributor.authorLisenfeld, U.
dc.contributor.authorBraine, J.
dc.contributor.authorBrinks, E.
dc.contributor.authorIglesias-Paramo, J.
dc.contributor.authorXi, C.K.
dc.date.accessioned2009-05-26T07:58:02Z
dc.date.available2009-05-26T07:58:02Z
dc.date.issued2009
dc.identifier.citationBoquien , M , Duc , P A , Wu , Y , Charmandaris , V , Lisenfeld , U , Braine , J , Brinks , E , Iglesias-Paramo , J & Xi , C K 2009 , ' Collisional Debris as Laboratories to Study Star Formation ' , The Astronomical Journal , vol. 137 , no. 6 , pp. 4561-4576 . https://doi.org/10.1088/0004-6256/137/6/4561
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 172894
dc.identifier.otherPURE UUID: 3c9e751d-816f-440f-b905-b3517c5d17a6
dc.identifier.otherdspace: 2299/3429
dc.identifier.otherScopus: 73049096721
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407841
dc.identifier.urihttp://hdl.handle.net/2299/3429
dc.descriptionOriginal article can be found at: http://www.iop.org/EJ/journal/1538-3881 Copyright American Astronomical Society. DOI: 10.1088/0004-6256/137/6/4561 [Full text of this article is not available in the UHRA]
dc.description.abstractIn this paper we address the question of whether star formation (SF) is driven by local processes or the large-scale environment. To do so, we investigate SF in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on SF in noninteracting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of six interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions (1) the emission of the dust is at the expected level for their luminosity and metallicity, (2) the usual tracers of SFR display the typical trend and scatter found in classical star-forming regions, and (3) the extinction and metallicity are not the main parameters governing the scatter in the properties of intergalactic star-forming regions; age effects and variations in the number of stellar populations seem to play an important role. Our work suggests that local properties such as column density and dust content, rather than the large-scale environment seem to drive SF. This means that intergalactic star-forming regions can be used as a reliable tool to study SF.en
dc.language.isoeng
dc.relation.ispartofThe Astronomical Journal
dc.titleCollisional Debris as Laboratories to Study Star Formationen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-6256/137/6/4561
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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