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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/20.500.12386/31308
DC FieldValueLanguage
dc.contributor.authorPessa, I.en_US
dc.contributor.authorSchinnerer, E.en_US
dc.contributor.authorBELFIORE, FRANCESCO MICHEL CONCETTOen_US
dc.contributor.authorEmsellem, E.en_US
dc.contributor.authorLeroy, A. K.en_US
dc.contributor.authorSchruba, A.en_US
dc.contributor.authorKruijssen, J. M. D.en_US
dc.contributor.authorPan, H. -A.en_US
dc.contributor.authorBlanc, G. A.en_US
dc.contributor.authorSanchez-Blazquez, P.en_US
dc.contributor.authorBigiel, F.en_US
dc.contributor.authorChevance, M.en_US
dc.contributor.authorCongiu, E.en_US
dc.contributor.authorDale, D.en_US
dc.contributor.authorFaesi, C. M.en_US
dc.contributor.authorGlover, S. C. O.en_US
dc.contributor.authorGrasha, K.en_US
dc.contributor.authorGroves, B.en_US
dc.contributor.authorHo, I.en_US
dc.contributor.authorJiménez-Donaire, M.en_US
dc.contributor.authorKlessen, R.en_US
dc.contributor.authorKreckel, K.en_US
dc.contributor.authorKoch, E. W.en_US
dc.contributor.authorLiu, D.en_US
dc.contributor.authorMeidt, S.en_US
dc.contributor.authorPety, J.en_US
dc.contributor.authorQuerejeta, M.en_US
dc.contributor.authorRosolowsky, E.en_US
dc.contributor.authorSaito, T.en_US
dc.contributor.authorSantoro, F.en_US
dc.contributor.authorSun, J.en_US
dc.contributor.authorUsero, A.en_US
dc.contributor.authorWatkins, E. J.en_US
dc.contributor.authorWilliams, T. G.en_US
dc.date.accessioned2022-01-05T09:27:01Z-
dc.date.available2022-01-05T09:27:01Z-
dc.date.issued2021en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/31308-
dc.description.abstractAims: The complexity of star formation at the physical scale of molecular clouds is not yet fully understood. We investigate the mechanisms regulating the formation of stars in different environments within nearby star-forming galaxies from the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) sample. Methods: Integral field spectroscopic data and radio-interferometric observations of 18 galaxies were combined to explore the existence of the resolved star formation main sequence (Σ<SUB>stellar</SUB> versus Σ<SUB>SFR</SUB>), resolved Kennicutt-Schmidt relation (Σ<SUB>mol. gas</SUB> versus Σ<SUB>SFR</SUB>), and resolved molecular gas main sequence (Σ<SUB>stellar</SUB> versus Σ<SUB>mol. gas</SUB>), and we derived their slope and scatter at spatial resolutions from 100 pc to 1 kpc (under various assumptions). <BR /> Results: All three relations were recovered at the highest spatial resolution (100 pc). Furthermore, significant variations in these scaling relations were observed across different galactic environments. The exclusion of non-detections has a systematic impact on the inferred slope as a function of the spatial scale. Finally, the scatter of the Σ<SUB>mol. gas + stellar</SUB> versus Σ<SUB>SFR</SUB> correlation is smaller than that of the resolved star formation main sequence, but higher than that found for the resolved Kennicutt-Schmidt relation. <BR /> Conclusions: The resolved molecular gas main sequence has the tightest relation at a spatial scale of 100 pc (scatter of 0.34 dex), followed by the resolved Kennicutt-Schmidt relation (0.41 dex) and then the resolved star formation main sequence (0.51 dex). This is consistent with expectations from the timescales involved in the evolutionary cycle of molecular clouds. Surprisingly, the resolved Kennicutt-Schmidt relation shows the least variation across galaxies and environments, suggesting a tight link between molecular gas and subsequent star formation. The scatter of the three relations decreases at lower spatial resolutions, with the resolved Kennicutt-Schmidt relation being the tightest (0.27 dex) at a spatial scale of 1 kpc. Variation in the slope of the resolved star formation main sequence among galaxies is partially due to different detection fractions of Σ<SUB>SFR</SUB> with respect to Σ<SUB>stellar</SUB>.en_US
dc.language.isoengen_US
dc.titleStar formation scaling relations at ∼100 pc from PHANGS: Impact of completeness and spatial scaleen_US
dc.typeArticle-
dc.identifier.doi10.1051/0004-6361/202140733en_US
dc.identifier.scopus2-s2.0-85108543509en_US
dc.identifier.urlhttps://www.aanda.org/articles/aa/full_html/2021/06/aa40733-21/aa40733-21.htmlen_US
dc.identifier.urlhttp://arxiv.org/abs/2104.09536v3en_US
dc.relation.mediumSTAMPAen_US
dc.relation.volume650en_US
dc.relation.firstpageA134en_US
dc.type.refereeREF_1en_US
dc.relation.scientificsectorFIS/05 - ASTRONOMIA E ASTROFISICAen_US
dc.relation.journalASTRONOMY & ASTROPHYSICSen_US
dc.type.miur262 Articolo in rivista-
dc.identifier.adsbibcode2021A&A...650A.134Pen_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.openairetypeArticle-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.languageiso639-1en-
item.cerifentitytypePublications-
item.fulltextWith Fulltext-
crisitem.journal.journalissn0004-6361-
crisitem.journal.anceE016240-
crisitem.author.deptO.A. Arcetri-
crisitem.author.orcid0000-0002-2545-5752-
Appears in Collections:1.01 Articoli in rivista
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2104.09536.pdfpostprint3.28 MBAdobe PDFView/Open
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