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Collisional debris as laboratories to study star formation

hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorBOQUIEN, M.
hal.structure.identifierDépartement d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée [DAPNIA]
dc.contributor.authorDUC, P. -A.
hal.structure.identifierNational Laboratory of Pattern Recognition [Beijing] [NLPR]
dc.contributor.authorWU, Y.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorCHARMANDARIS, V.
hal.structure.identifierDepartamento Física Teórica y del Cosmos
dc.contributor.authorLISENFELD, U.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBRAINE, J.
hal.structure.identifierCentre for Astrophysics Research
dc.contributor.authorBRINKS, E.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorIGLESIAS-PÁRAMO, J.
hal.structure.identifierLaboratoire de Mathématiques Raphaël Salem [LMRS]
dc.contributor.authorXU, C. K.
dc.date.created2009
dc.date.issued2009
dc.identifier.issn0004-6256
dc.description.abstractEnIn this paper we address the question whether star formation is driven by local processes or the large scale environment. To do so, we investigate star formation in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on star formation in non-interacting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of 6 interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions a) the emission of the dust is at the expected level for their luminosity and metallicity, b) the usual tracers of star formation rate display the typical trend and scatter found in classical star forming regions, and c) 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 star formation. This means that intergalactic star forming regions can be used as a reliable tool to study star formation.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enultraviolet: galaxies
dc.subject.engalaxies: dwarf
dc.subject.engalaxies: interactions
dc.subject.engalaxies: irregular
dc.subject.eninfrared: galaxies
dc.subject.enstars: formation
dc.title.enCollisional debris as laboratories to study star formation
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-6256/137/6/4561
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv0903.3403
bordeaux.journalThe Astronomical Journal
bordeaux.page4561-4576
bordeaux.volume137
bordeaux.issue6
bordeaux.peerReviewedoui
hal.identifierhal-00401169
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00401169v1
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