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Velocity resolved [CII] spectroscopy of the center and the BCLMP302 region of M33 (HerM33es)

hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorMOOKERJEA, B.,
dc.contributor.authorISRAEL, F.,
dc.contributor.authorKRAMER, C.,
dc.contributor.authorNIKOLA, T.,
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorBRAINE, J.
dc.contributor.authorOSSENKOPF, V.,
hal.structure.identifierKOSMA,
dc.contributor.authorROELLIG, M.,
dc.contributor.authorHENKEL, C.,
dc.contributor.authorVAN DER WERF, P.,
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorVAN DER TAK, F.,
hal.structure.identifierObservatoire de Paris
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorWIEDNER, M. C.,
dc.date.issued2016
dc.identifier.issn0004-6361
dc.description.abstractEnWe aim to understand the contribution of the ionized, atomic and molecular phases of the ISM to the [CII] emission from clouds near the dynamical center and the BCLMP302 HII region in the north of the nearby galaxy M33 at a spatial resolution of 50pc. We combine high resolution [CII] spectra taken with the HIFI spectrometer onboard the Herschel satellite with [CII] Herschel-PACS maps and ground-based observations of CO(2-1) and HI. All data are at a common spatial resolution of 50pc. Typically, the [CII] lines have widths intermediate between the narrower CO(2-1) and broader HI line profiles. We decomposed the [CII] spectra in terms of contribution from molecular and atomic gas detected in CO(2-1) and HI, respectively. We find that the relative contribution of molecular and atomic gas traced by CO(2-1) and HI varies depends mostly on the local physical conditions and geometry. We estimate that 11-60% and 5-34% of the [CII] intensities in the center and in BCLMP302, respectively, arise at velocities showing no CO(2-1) or HI emission and could arise in CO-dark molecular gas. The deduced strong variation in the [CII] emission not associated with CO and HI cannot be explained in terms of differences in A_v, far-ultraviolet radiation field, and metallicity between the two studied regions. Hence the relative amounts of diffuse (CO-dark) and dense molecular gas possibly vary on spatial scales smaller than 50pc. Based on the emission measure observed at radio wavelengths we estimate the contribution of ionized gas at a few positions to lie between 10-25%. The correlations between the intensities of tracers corresponding to the same velocity range as [CII], differ from the correlation derived from PACS data. The results in this paper emphasize the need for velocity-resolved observations to discern the contribution of different components of the ISM to [CII] emission. (abridged)
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enVelocity resolved [CII] spectroscopy of the center and the BCLMP302 region of M33 (HerM33es)
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201527366
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1512.00904
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A37
bordeaux.volume586
bordeaux.peerReviewedoui
hal.identifierhal-01238993
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01238993v1
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