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Bipolar H II regions - Morphology and star formation in their vicinity I. G319.88+00.79 and G010.32-00.15

hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorDEHARVENG, L.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorZAVAGNO, Annie
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorSAMAL, M. R.
hal.structure.identifierNational Radio Astronomy Observatory [Green Bank] [NRAO]
hal.structure.identifierDepartment of Physics and Astronomy [Morgantown]
dc.contributor.authorANDERSON, L. D.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorLELEU, G.
dc.contributor.authorBREVOT, D.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierUniversité Sciences et Technologies - Bordeaux 1 [UB]
hal.structure.identifierFORMATION STELLAIRE 2014
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorDUARTE-CABRAL, A.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorMOLINARI, S.
dc.contributor.authorPESTALOZZI, M.
dc.contributor.authorFOSTER, J. B.
dc.contributor.authorRATHBORNE, J. M.
dc.contributor.authorJACKSON, J. M.
dc.date.issued2015-10
dc.identifier.issn0004-6361
dc.description.abstractEnAims. Our goal is to identify bipolar H II regions and to understand their morphology, their evolution, and the role they play in the formation of new generations of stars. Methods. We use the Spitzer-GLIMPSE, -MIPSGAL, and Herschel-Hi-GAL surveys to identify bipolar H II regions, looking for (ionized) lobes extending perpendicular to dense filamentary structures. We search for their exciting star(s) and estimate their distances using near-IR data from the 2MASS or UKIDSS surveys. Dense molecular clumps are detected using Herschel-SPIRE data, and we estimate their temperature, column density, mass, and density. MALT90 observations allow us to ascertain their association with the central H II region (association based on similar velocities). We identify Class 0/I young stellar objects (YSOs) using their Spitzer and Herschel-PACS emissions. These methods will be applied to the entire sample of candidate bipolar H II regions to be presented in a forthcoming paper. Results. This paper focuses on two bipolar H II regions, one that is especially interesting in terms of its morphology, G319.88+00.79, and one in terms of its star formation, G010.32-00.15. Their exciting clusters are identified and their photometric distances estimated to be 2.6 kpc and 1.75 kpc, respectively; thus G010.32-00.15 (known as W31 north) lies much closer than previously assumed. We suggest that these regions formed in dense and flat structures that contain filaments. They have a central ionized region and ionized lobes extending perpendicular to the parental cloud. The remains of the parental cloud appear as dense (more than 10(4) cm(-3)) and cold (14-17 K) condensations. The dust in the photodissociation regions (in regions adjacent to the ionized gas) is warm (19-25 K). Dense massive clumps are present around the central ionized region. G010.32-00.14 is especially remarkable because five clumps of several hundred solar masses surround the central H II region; their peak column density is a few 10(23) cm(-2), and the mean density in their central regions reaches several 10(5) cm(-3). Four of them contain at least one massive YSO (including an ultracompact H II region and a high-luminosity Class I YSO); these clumps also contain extended green objects (EGOs) and Class II methanol masers. This morphology suggests that the formation of a second generation of massive stars has been triggered by the central bipolar H II region. It occurs in the compressed material of the parental cloud.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enBipolar H II regions - Morphology and star formation in their vicinity I. G319.88+00.79 and G010.32-00.15
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201423835
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1507.00215
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.volume582
bordeaux.peerReviewedoui
hal.identifierhal-01439774
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01439774v1
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