Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26855
DC Field | Value | Language |
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dc.contributor.author | Tigé, J. | en_US |
dc.contributor.author | Motte, F. | en_US |
dc.contributor.author | Russeil, D. | en_US |
dc.contributor.author | Zavagno, A. | en_US |
dc.contributor.author | Hennemann, M. | en_US |
dc.contributor.author | Schneider, N. | en_US |
dc.contributor.author | Hill, T. | en_US |
dc.contributor.author | Nguyen Luong, Q. | en_US |
dc.contributor.author | Di Francesco, J. | en_US |
dc.contributor.author | Bontemps, S. | en_US |
dc.contributor.author | Louvet, F. | en_US |
dc.contributor.author | Didelon, P. | en_US |
dc.contributor.author | Könyves, V. | en_US |
dc.contributor.author | André, Ph. | en_US |
dc.contributor.author | Leuleu, G. | en_US |
dc.contributor.author | Bardagi, J. | en_US |
dc.contributor.author | Anderson, L. D. | en_US |
dc.contributor.author | Arzoumanian, D. | en_US |
dc.contributor.author | BENEDETTINI, Milena | en_US |
dc.contributor.author | Bernard, J. -P. | en_US |
dc.contributor.author | ELIA, Davide Quintino | en_US |
dc.contributor.author | Figueira, M. | en_US |
dc.contributor.author | Kirk, J. | en_US |
dc.contributor.author | Martin, P. G. | en_US |
dc.contributor.author | Minier, V. | en_US |
dc.contributor.author | MOLINARI, Sergio | en_US |
dc.contributor.author | Nony, T. | en_US |
dc.contributor.author | Persi, P. | en_US |
dc.contributor.author | PEZZUTO, Stefano | en_US |
dc.contributor.author | Polychroni, D. | en_US |
dc.contributor.author | Rayner, T. | en_US |
dc.contributor.author | Rivera-Ingraham, A. | en_US |
dc.contributor.author | Roussel, H. | en_US |
dc.contributor.author | RYGL, Kazi Lucie Jessica | en_US |
dc.contributor.author | SPINOGLIO, Luigi Giuseppe Maria | en_US |
dc.contributor.author | White, G. J. | en_US |
dc.date.accessioned | 2020-08-27T08:16:13Z | - |
dc.date.available | 2020-08-27T08:16:13Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26855 | - |
dc.description.abstract | Aims: To constrain models of high-mass star formation, the Herschel-HOBYS key program aims at discovering massive dense cores (MDCs) able to host the high-mass analogs of low-mass prestellar cores, which have been searched for over the past decade. We here focus on NGC 6334, one of the best-studied HOBYS molecular cloud complexes. <BR /> Methods: We used Herschel/PACS and SPIRE 70-500 μm images of the NGC 6334 complex complemented with (sub)millimeter and mid-infrared data. We built a complete procedure to extract 0.1 pc dense cores with the getsources software, which simultaneously measures their far-infrared to millimeter fluxes. We carefully estimated the temperatures and masses of these dense cores from their spectral energy distributions (SEDs). We also identified the densest pc-scale cloud structures of NGC 6334, one 2 pc × 1 pc ridge and two 0.8 pc × 0.8 pc hubs, with volume-averaged densities of 10<SUP>5</SUP> cm<SUP>-3</SUP>. <BR /> Results: A cross-correlation with high-mass star formation signposts suggests a mass threshold of 75 M<SUB>☉</SUB> for MDCs in NGC 6334. MDCs have temperatures of 9.5-40 K, masses of 75-1000 M<SUB>☉</SUB>, and densities of 1 × 10<SUP>5</SUP>-7 × 10<SUP>7</SUP> cm<SUP>-3</SUP>. Their mid-infrared emission is used to separate 6 IR-bright and 10 IR-quiet protostellar MDCs while their 70 μm emission strength, with respect to fitted SEDs, helps identify 16 starless MDC candidates. The ability of the latter to host high-mass prestellar cores is investigated here and remains questionable. An increase in mass and density from the starless to the IR-quiet and IR-bright phases suggests that the protostars and MDCs simultaneously grow in mass. The statistical lifetimes of the high-mass prestellar and protostellar core phases, estimated to be 1-7 × 10<SUP>4</SUP> yr and at most 3 × 10<SUP>5</SUP> yr respectively, suggest a dynamical scenario of high-mass star formation. <BR /> Conclusions: The present study provides good mass estimates for a statistically significant sample, covering the earliest phases of high-mass star formation. High-mass prestellar cores may not exist in NGC 6334, favoring a scenario presented here, which simultaneously forms clouds, ridges, MDCs, and high-mass protostars. <P />Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Catalogs built from Tables A.1-A.12, are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/602/A77">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/602/A77 | en_US |
dc.language.iso | eng | en_US |
dc.title | The earliest phases of high-mass star formation, as seen in NGC 6334 by Herschel-HOBYS | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201628989 | en_US |
dc.identifier.scopus | 2-s2.0-85021057443 | en_US |
dc.identifier.isi | 000404648300013 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2017/06/aa28989-16/aa28989-16.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 602 | en_US |
dc.relation.firstpage | A77 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | CAN | 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 | 2017A&A...602A..77T | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare 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.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.orcid | 0000-0002-3597-7263 | - |
crisitem.author.orcid | 0000-0002-9120-5890 | - |
crisitem.author.orcid | 0000-0002-9826-7525 | - |
crisitem.author.orcid | 0000-0001-7852-1971 | - |
crisitem.author.orcid | 0000-0003-4146-9043 | - |
crisitem.author.orcid | 0000-0001-8840-1551 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
tige2017.pdf | PDF editoriale | 72.85 MB | Adobe PDF | View/Open |
aa28989-16 compr.pdf | Miur | 6.86 MB | Adobe PDF |
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