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The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302

hal.structure.identifierKOSMA, I. Physikalisches Institut
dc.contributor.authorMOOKERJEA, B.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorKRAMER, C.
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.identifierDept. fısica Teorica y del Cosmos
dc.contributor.authorVERLEY, S.
hal.structure.identifierDpto. Fisica Teorica y del Cosmos
dc.contributor.authorRELANO, M.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorQUINTANA-LACACI, G.
dc.contributor.authorAALTO, S.
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.authorBRAINE, J.
hal.structure.identifierDepartment of Astronomy
dc.contributor.authorCALZETTI, D.
dc.contributor.authorCOMBES, F.
hal.structure.identifierObservatorio Astronomico Nacional, Madrid
dc.contributor.authorGARCIA-BURILLO, S.
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.authorGRATIER, P.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorHENKEL, C.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorISRAEL, F.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorLORD, S.
dc.contributor.authorNIKOLA, T.
hal.structure.identifierKOSMA,
dc.contributor.authorROELLIG, M.
dc.contributor.authorSTACEY, G.
dc.contributor.authorTABATABAEI, F. S.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorVAN DER TAK, F.
dc.contributor.authorVAN DER WERF, P.
dc.date.created2011-06-27
dc.date.issued2011
dc.identifier.issn0004-6361
dc.description.abstractEnContext: The emission line of [CII] at 158 micron is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Aims: Disentangling the relative contributions of the different ISM phases to [CII] emission, is a major topic of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Methods: Using PACS, we have mapped the emission of [CII] 158 micron, [OI] 63 micron, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of H-alpha emission, we have observed in addition a velocity resolved [CII] spectrum using HIFI. We use scatterplots to compare these data with PACS 160 micron continuum maps, and with maps of CO and HI data, at a common resolution of 12 arcsec or 50 pc. Maps of H-alpha and 24 micron emission observed with Spitzer are used to estimate the SFR. We have created maps of the [CII] and [OI] 63 micron emission and detected [NII] 122 micron and NIII 57 micron at individual positions. Results: The [CII] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [CII] observed with PACS and CO over the mapped region. There is even less spatial correlation between [CII] and the atomic gas traced by HI. Detailed comparison of the observed intensities towards the HII region with models of photo ionization and photon dominated regions, confirms that a significant fraction, 20--30%, of the observed [CII] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio between [CII] and the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the HII region.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enThe Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201116447
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]
dc.identifier.arxiv1106.5464
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA152
bordeaux.volume532
bordeaux.peerReviewedoui
hal.identifierhal-00605980
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00605980v1
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