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Spectrally resolved CII emission in M~33 ({\tt HerM33es}): Physical conditions and kinematics around BCLMP 691

hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBRAINE, J.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorGRATIER, P.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorKRAMER, C.
dc.contributor.authorISRAEL, F. P.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorVAN DER TAK, F.
hal.structure.identifierKOSMA, I. Physikalisches Institut
dc.contributor.authorMOOKERJEA, B.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierDepartment of Astronomy
dc.contributor.authorBOQUIEN, M.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorTABATABAEI, F.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DER WERF, P.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorHENKEL, C.
dc.date.created2012-07-13
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnThis work presents high spectral resolution observations of the \CII\ line at 158 \micron, one of the major cooling lines of the interstellar medium, taken with the HIFI heterodyne spectrometer on the Herschel satellite. In BCLMP 691, an \HII\ region far north (3.3 kpc) in the disk of M 33, the \CII\ and CO line profiles show similar velocities within $0.5 \kms$, while the \HI\ line velocities are systematically shifted towards lower rotation velocities by $\sim 5\kms$. Observed at the same $12"$ angular resolution, the \CII\ lines are broader than those of CO by about 50% but narrower than the \HI\ lines. The \CII\ line to far-infrared continuum ratio suggests a photoelectric heating efficiency of 1.1%. The data, together with published models indicate a UV field $G_0 \sim 100$ in units of the solar neighborhood value, a gas density $n_H \sim 1000 \cc$, and a gas temperature $T\sim 200$ K. Adopting these values, we estimate the C$^+$ column density to be $N_{C^+} \approx 1.3 \times 10^{17} \cmt$. The \CII\ emission comes predominantly from the warm neutral region between the \HII\ region and the cool molecular cloud behind it. From published abundances, the inferred C$^+$ column corresponds to a hydrogen column density of $N_H \sim 2 \times 10^{21} \cmt$. The CO observations suggest that $N_H = 2 N_{H_2} \sim 3.2 \times 10^{21} \cmt$ and 21cm measurements, also at $12"$ resolution, yield $N_\HI \approx 1.2 \times 10^{21} \cmt$ within the \CII\ velocity range. Thus, some H$_2$ not detected in CO must be present, in agreement with earlier findings based on the SPIRE 250 -- 500 $\mu$m emission.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enSpectrally resolved CII emission in M~33 ({\tt HerM33es}): Physical conditions and kinematics around BCLMP 691
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201219360
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.arxiv1207.3243
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A55
bordeaux.volume544
bordeaux.peerReviewedoui
hal.identifierhal-00718466
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00718466v1
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