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The clumpy structure of the chemically active L1157 outflow

dc.contributor.authorBENEDETTINI, Milena
dc.contributor.authorVITI, Serena
dc.contributor.authorCODELLA, Claudio
dc.contributor.authorBACHILLER, Rafael
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorGUETH, Frederic
hal.structure.identifierDepartamento de Fisica Teorica
dc.contributor.authorBELTRÀN, Maria T.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
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.authorDUTREY, Anne
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.authorGUILLOTEAU, S.
dc.date.created2007
dc.date.issued2007
dc.identifier.issn0035-8711
dc.description.abstractEnWe present high spatial resolution maps, obtained with the Plateau de Bure Interferometer, of the blue lobe of the L1157 outflow. We observed four lines at 3 mm, namely CH3OH (2_K-1_K), HC3N (11-10), HCN (1-0) and OCS (7-6). Moreover, the bright B1 clump has also been observed at better spatial resolution in CS (2-1), CH3OH (2_1-1_1)A-, and 34SO (3_2-2_1). These high spatial resolution observations show a very rich structure in all the tracers, revealing a clumpy structure of the gas superimposed to an extended emission. In fact, the three clumps detected by previous IRAM-30m single dish observations have been resolved into several sub-clumps and new clumps have been detected in the outflow. The clumps are associated with the two cavities created by two shock episodes driven by the precessing jet. In particular, the clumps nearest the protostar are located at the walls of the younger cavity with a clear arch-shape form while the farthest clumps have slightly different observational characteristics indicating that they are associated to the older shock episode. The emission of the observed species peaks in different part of the lobe: the east clumps are brighter in HC3N (11-10), HCN (1-0) and CS (2-1) while the west clumps are brighter in CH3OH(2_K-1_K), OCS (7-6) and 34SO (3_2-2_1). This peak displacement in the line emission suggests a variation of the physical conditions and/or the chemical composition along the lobe of the outflow at small scale, likely related to the shock activity and the precession of the outflow. In particular, we observe the decoupling of the silicon monoxide and methanol emission, common shock tracers, in the B1 clump located at the apex of the bow shock produced by the second shock episode.
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.title.enThe clumpy structure of the chemically active L1157 outflow
dc.typeArticle de revue
dc.identifier.doi10.1111/j.1365-2966.2007.12300.x
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv0708.0133
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page1127-1136
bordeaux.volume381
bordeaux.issue3
bordeaux.peerReviewedoui
hal.identifierhal-00265889
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00265889v1
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