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Cool gas and dust in M33: Results from the Herschel M33 extended survey (HERM33ES)

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]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorBRAINE, J.
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]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorGRATIER, P.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorKRAMER, C.
hal.structure.identifierInstitute of Astronomy and Astrophysics,
dc.contributor.authorXILOURIS, E.M.
hal.structure.identifierUniversity of British Columbia [UBC]
dc.contributor.authorROSOLOWSKY, E.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorBUCHBENDER, C.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierDepartment of Astronomy
dc.contributor.authorBOQUIEN, M.
hal.structure.identifierDepartment of Astronomy
dc.contributor.authorCALZETTI, D.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorQUINTANA-LACACI, G.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorTABATABAEI, F.
hal.structure.identifierDept. fısica Teorica y del Cosmos
dc.contributor.authorVERLEY, S.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorISRAEL, F.
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorVAN DER TAK, Floris
hal.structure.identifierTKK Helsinki University of Technology [TKK]
dc.contributor.authorAALTO, Samuli
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorCOMBES, F.
hal.structure.identifierObservatorio Astronomico Nacional, Madrid
dc.contributor.authorGARCIA-BURILLO, S.
hal.structure.identifierFundación Venezolana de Investigaciones Sismológicas [FUNVISIS]
hal.structure.identifierInstituto de Ciencias de la Tierra
dc.contributor.authorGONZALEZ, M.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorHENKEL, Carsten
hal.structure.identifierAustralia Telescope National Facility
dc.contributor.authorKORIBALSKI, B.
hal.structure.identifierKOSMA, I. Physikalisches Institut
dc.contributor.authorMOOKERJEA, B.
hal.structure.identifierKOSMA,
dc.contributor.authorROELLIG, M.
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorSCHUSTER, K. F.
hal.structure.identifierDpto. Fisica Teorica y del Cosmos
dc.contributor.authorRELANO, M.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorBERTOLDI, F.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DER WERF, Paul
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorWIEDNER, M.
dc.date.created2010
dc.date.issued2010
dc.identifier.issn0004-6361
dc.description.abstractEnWe present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H2 content. In this Letter, we measure the dust emission cross-section using SPIRE and recent CO and Hi observations; a variation in is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the Hi column, yields amorphology similar to that observed in CO. The H2/Hi mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enGalaxies: Individual: M 33
dc.subject.enGalaxies: Local Group
dc.subject.enGalaxies: evolution
dc.subject.enGalaxies: ISM
dc.subject.enISM: Clouds
dc.subject.enStars: Formation
dc.title.enCool gas and dust in M33: Results from the Herschel M33 extended survey (HERM33ES)
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201014551
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL69
bordeaux.volume518
bordeaux.peerReviewedoui
hal.identifierhal-00484750
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00484750v1
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