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W43: the closest molecular complex of the Galactic Bar?

dc.contributor.authorLUONG, Q. Nguyen
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierInstitut de Recherches sur les lois Fondamentales de l'Univers [IRFU]
dc.contributor.authorMOTTE, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorSCHULLER, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierUniversité Sciences et Technologies - Bordeaux 1 [UB]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorSCHILKE, P.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorMENTEN, K. M.
dc.contributor.authorHEITSCH, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
dc.contributor.authorCARLHOFF, P.
hal.structure.identifierDepartamento de Astronomia [DAS]
dc.contributor.authorBRONFMAN, L.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, T.
dc.date.created2011-02-19
dc.date.issued2011
dc.identifier.issn0004-6361
dc.description.abstractEnWe used a large database extracted from Galaxy-wide surveys of H {\scriptsize I}, $^{13}$CO 1-0, $8 \micron$ and $870 \micron$ continuum to trace diffuse atomic gas, low- to medium-density molecular gas, high-density molecular gas, and star formation activity which we complemented by dedicated $^{12}$CO 2--1, 3--2 observations of the W43 region. From the detailed 3D (space-space-velocity) analysis of the molecular and atomic cloud tracers through the region and despite its wide velocity range (\emph{FWHM}$\sim22.3 \kms$ around $\vlsr\sim 95.9 \kms$), we identified W43 as a large (equivalent diameter $\sim 140$ pc) and coherent complex of molecular clouds which is surrounded by an atomic gas envelope (equivalent diameter $\sim 290$ pc). We measured the total mass of this newly-identified molecular complex ($M_{{\tiny total}}\sim 7.1 \times 10^6 \msun$), the mass contained in dense $870 \micron$ clumps ($<5$ pc dense cloud structures, $M_{{\tiny clumps}}\sim 8.4 \times 10^5 \msun$) and conclude that W43 is particularly massive and concentrated. The distance we assume for the W43 complex is 6 kpc from the Sun, which may place it at the meeting point of the Scutum-Centaurus (or Scutum-Crux) Galactic arm and the Bar, a dynamically complex region where high-velocity streams could easily collide. The star formation rate of W43 is suggested not to be steady but it is increasing from $\, \sim 0.01 \msun\, {yr}^{-1}$ (measured from its $8\,\mu$m luminosity) to $\sim 0.1 \msun\, {yr}^{-1}$ (measured from its molecular content). From the global properties of W43, we claim it is an extreme molecular complex in the Milky Way and it could even be forming starburst clusters in the near future.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enSolar and Stellar Astrophysics
dc.title.enW43: the closest molecular complex of the Galactic Bar?
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201016271
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1102.3460
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA41
bordeaux.volume529
bordeaux.peerReviewedoui
hal.identifierhal-00570350
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00570350v1
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