Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/24043
Campo DC | Valore | Lingua |
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dc.contributor.author | Deharveng, L. | en_US |
dc.contributor.author | Zavagno, A. | en_US |
dc.contributor.author | Samal, M. R. | en_US |
dc.contributor.author | Anderson, L. D. | en_US |
dc.contributor.author | LeLeu, G. | en_US |
dc.contributor.author | Brevot, D. | en_US |
dc.contributor.author | Duarte-Cabral, A. | en_US |
dc.contributor.author | MOLINARI, Sergio | en_US |
dc.contributor.author | Pestalozzi, M. | en_US |
dc.contributor.author | Foster, J. B. | en_US |
dc.contributor.author | Rathborne, J. M. | en_US |
dc.contributor.author | Jackson, J. M. | en_US |
dc.date.accessioned | 2020-04-15T13:26:52Z | - |
dc.date.available | 2020-04-15T13:26:52Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/24043 | - |
dc.description.abstract | Aims: 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) 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, and the mean density in their central regions reaches several. 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. Appendices are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201423835/olm">http://www.aanda.org | en_US |
dc.language.iso | eng | en_US |
dc.title | Bipolar H II regions - Morphology and star formation in their vicinity. I. G319.88+00.79 and G010.32-00.15 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201423835 | en_US |
dc.identifier.scopus | 2-s2.0-84942806478 | en_US |
dc.identifier.isi | 000363538500001 | en_US |
dc.identifier.url | http://arxiv.org/abs/1507.00215v1 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2015/10/aa23835-14/aa23835-14.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 582 | en_US |
dc.relation.firstpage | A1 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015A&A...582A...1D | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.orcid | 0000-0002-9826-7525 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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File | Descrizione | Dimensioni | Formato | |
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aa23835-14.pdf | PDF editoriale | 10.34 MB | Adobe PDF | Visualizza/apri |
24043-aa23835-14_P01.pdf | Miur | 8.9 MB | Adobe PDF | |
24043-aa23835-14_P02.pdf | Miur | 1.46 MB | Adobe PDF |
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