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Coupling the dynamics and the molecular chemistry in the Galactic center

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]
hal.structure.identifierUniversité Sciences et Technologies - Bordeaux 1 [UB]
dc.contributor.authorRODRIGUEZ‐FERNANDEZ, Nemesio
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorCOMBES, F.
hal.structure.identifierInstituto de Estructura de la Materia [IEM]
dc.contributor.authorMARTIN-PINTADO, Jesus
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorWILSON, Thomas
hal.structure.identifierUniversity of Arizona
dc.contributor.authorAPPONI, Aldo
dc.date.issued2006
dc.identifier.issn0004-6361
dc.description.abstractEnThe physical conditions of the Galactic center (GC) clouds moving with non-circular velocities are not well-known. We have studied the physical conditions of these clouds with the aim of better understanding the origin of the outstanding physical conditions of the GC molecular gas and the possible effect of the large scale dynamics on these physical conditions.Using published CO(1-0) data, we have selected a set of clouds belonging to all the kinematical components seen in the longitude-velocity diagram of the GC. We have done a survey of dense gas in all the components using the J=2-1 lines of CS and SiO as tracers of high density gas and shock chemistry. We have detected CS and SiO emission in all the kinematical components. The gas density and the SiO abundance of the clouds in non-circular orbits are similar those in the nuclear ring (GCR). Therefore, in all the kinematical components there are dense clouds that can withstand the tidal shear. However, there is no evidence of star formation outside the GCR. The high relative velocity and shear expected in the dust-lanes along the bar major axis could inhibit the star formation process, as observed in other galaxies. The high SiO abundances derived in the non-circular velocity clouds are likely due to the large-scale shocks that created the dust lanes
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enISM: kinematics and dynamics
dc.subject.enISM: molecules
dc.subject.enGalaxy: center
dc.subject.enGalaxies: ISM
dc.subject.enRadio lines : ISM
dc.title.enCoupling the dynamics and the molecular chemistry in the Galactic center
dc.typeArticle de revue
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page963-969
bordeaux.volume455
bordeaux.peerReviewedoui
hal.identifierhal-00022039
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00022039v1
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