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The Dust Properties of Bubble HII Regions as seen by Herschel

dc.contributor.authorANDERSON, L. D.
dc.contributor.authorZAVAGNO, Annie
dc.contributor.authorDEHARVENG, L.
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorABERGEL, A.
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.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRE, Ph.
dc.contributor.authorBERNARD, J. -P.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHENNEMANN, M.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHILL, T.
dc.contributor.authorRODON, J. A.
dc.contributor.authorROUSSEL, Hervé
dc.contributor.authorRUSSEIL, D.
dc.date.created2012-03-26
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnBecause of their relatively simple morphology, "bubble" HII regions have been instrumental to our understanding of star formation triggered by HII regions. With the far-infrared (FIR) spectral coverage of the Herschel satellite, we can access the wavelengths where these regions emit the majority of their energy through their dust emission. At Herschel wavelengths 70 micron to 500 micron, the emission associated with HII regions is dominated by the cool dust in their photodissociation regions (PDRs). We find average dust temperatures of 26K along the PDRs, with little variation between the HII regions in the sample, while local filaments and infrared dark clouds average 19K and 15K respectively. Higher temperatures lead to higher values of the Jeans mass, which may affect future star formation. The mass of the material in the PDR, collected through the expansion of the HII region, is between ~300 and ~10,000 Solar masses for the HII regions studied here. These masses are in rough agreement with the expected masses swept up during the expansion of the \hii\ regions. Approximately 20% of the total FIR emission is from the direction of the bubble central regions. This suggests that we are detecting emission from the "near-side" and "far-side" PDRs along the line of sight and that bubbles are three-dimensional structures. We find only weak support for a relationship between dust temperature and beta, of a form similar to that caused by noise and calibration uncertainties alone.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enThe Dust Properties of Bubble HII Regions as seen by Herschel
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201117283
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.arxiv1203.5721
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA10
bordeaux.volume542
bordeaux.peerReviewedoui
hal.identifierhal-00683513
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00683513v1
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