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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/24560
DC FieldValueLanguage
dc.contributor.authorRagan, S. E.en_US
dc.contributor.authorMoore, T. J. T.en_US
dc.contributor.authorEden, D. J.en_US
dc.contributor.authorHoare, M. G.en_US
dc.contributor.authorELIA, Davide Quintinoen_US
dc.contributor.authorMOLINARI, Sergioen_US
dc.date.accessioned2020-05-06T14:57:03Z-
dc.date.available2020-05-06T14:57:03Z-
dc.date.issued2016en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/24560-
dc.description.abstractWe present large-scale trends in the distribution of star-forming objects revealed by the Hi-GAL survey. As a simple metric probing the prevalence of star formation in Hi-GAL sources, we define the fraction of the total number of Hi-GAL sources with a 70 μm counterpart as the `star-forming fraction' or SFF. The mean SFF in the inner galactic disc (3.1 kpc < R<SUB>GC</SUB> < 8.6 kpc) is 25 per cent. Despite an apparent pile-up of source numbers at radii associated with spiral arms, the SFF shows no significant deviations at these radii, indicating that the arms do not affect the star-forming productivity of dense clumps either via physical triggering processes or through the statistical effects of larger source samples associated with the arms. Within this range of Galactocentric radii, we find that the SFF declines with R<SUB>GC</SUB> at a rate of -0.026 ±0.002 per kiloparsec, despite the dense gas mass fraction having been observed to be constant in the inner Galaxy. This suggests that the SFF may be weakly dependent on one or more large-scale physical properties of the Galaxy, such as metallicity, radiation field, pressure or shear, such that the dense sub-structures of molecular clouds acquire some internal properties inherited from their environment.en_US
dc.language.isoengen_US
dc.titleThe prevalence of star formation as a function of Galactocentric radiusen_US
dc.typeArticle-
dc.identifier.doi10.1093/mnras/stw1870en_US
dc.identifier.scopus2-s2.0-84989208818en_US
dc.identifier.isi000384676000060en_US
dc.identifier.urlhttps://academic.oup.com/mnras/article/462/3/3123/2589928en_US
dc.relation.mediumELETTRONICOen_US
dc.relation.volume462en_US
dc.relation.issue3en_US
dc.relation.firstpage3123en_US
dc.type.refereeREF_1en_US
dc.relation.scientificsectorFIS/05 - ASTRONOMIA E ASTROFISICAen_US
dc.relation.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.type.miur262 Articolo in rivista-
dc.identifier.adsbibcode2016MNRAS.462.3123Ren_US
dc.description.apcnoen_US
dc.description.oa1 – prodotto con file in versione Open Access (allegare il file al passo  5-Carica)en_US
item.grantfulltextopen-
item.languageiso639-1en-
item.fulltextWith Fulltext-
item.openairetypeArticle-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.cerifentitytypePublications-
crisitem.journal.journalissn0035-8711-
crisitem.journal.anceE112946-
crisitem.author.deptIAPS Roma-
crisitem.author.deptIAPS Roma-
crisitem.author.orcid0000-0002-9120-5890-
crisitem.author.orcid0000-0002-9826-7525-
Appears in Collections:1.01 Articoli in rivista
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