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dc.contributor.authorVílchez, J M
dc.contributor.authorRelaño, M
dc.contributor.authorKennicutt, R
dc.contributor.authorDe Looze, I
dc.contributor.authorMollá, M
dc.contributor.authorGalametz, M
dc.date.accessioned2019-08-05T21:17:10Z
dc.date.available2019-08-05T21:17:10Z
dc.date.issued2019-03
dc.identifier.citationJ M Vílchez, M Relaño, R Kennicutt, I De Looze, M Mollá, M Galametz, Metals and dust content across the galaxies M 101 and NGC 628, Monthly Notices of the Royal Astronomical Society, Volume 483, Issue 4, March 2019, Pages 4968–4983, https://doi.org/10.1093/mnras/sty3455en_US
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/sty3455
dc.identifier.urihttp://hdl.handle.net/10150/633671
dc.description.abstractWe present a spatially resolved study of the relation between dust and metallicity in the nearby spiral galaxies M 101 (NGC 5457) and NGC 628 (M 74). We explore the relation between the chemical abundances of their gas and stars with their dust content and their chemical evolution. The empirical spatially resolved oxygen effective yield and the gas-to-dust mass ratio (GDR) across both disc galaxies are derived, sampling 1 dex in oxygen abundance. We find that the metal budget of the NGC 628 disc and most of the M 101 disc appears consistent with the predictions of the simple model of chemical evolution for an oxygen yield between half and one solar, whereas the outermost region (R >= 0.8 R-2(5)) of M 101 presents deviations suggesting the presence of gas flows. The GDR-metallicity relation shows a two slopes behaviour, with a break at 12 + log(O/H)P approximate to 8.4, a critical metallicity predicted by theoretical dust models when stardust production equals grain growth. A relation between GDR and the fraction of molecular to total gas, Sigma(H)(2)/Sigma(gas) is also found. We suggest an empirical relationship between GDR and the combination of 12 + log(O/H), for metallicity, and Sigma(H)(2)/Sigma(gas), a proxy for the molecular clouds fraction. The GDR is closely related with metallicity at low abundance and with Sigma(H)(2)/Sigma(gas) for higher metallicities suggesting interstellar medium dust growth. The ratio Sigma(star)/Sigma(dust) correlates well with 12 + log(O/H) and strongly with log(N/O) in both galaxies. For abundances below the critical one, the( )'stardust'( )production gives us a constant value suggesting a stellar dust yield similar to the oxygen yield.en_US
dc.description.sponsorshipSpanish Ministerio de Economia y Competitividad [AYA2016-79724-C4-4-P, AYA2016-79724-C4-3-P, AYA2014-53506-P, AYA2017-84897-P]; Junta de Andalucia (Spain) [PEX2011-FQM-7058]; Junta de Andalucia [FQM108]; European Regional Development Funds (FEDER); Spanish MECD [PRX17/00485]; MIAPP 2016 program 'The Chemical Evolution of Galaxies' of the Excellence Cluster 'Universe'en_US
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.rights© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.en_US
dc.subjectdust,extinctionen_US
dc.subjectISM: moleculesen_US
dc.subjectgalaxies: abundancesen_US
dc.subjectgalaxies: individual: NGC 5457 and NGC 628en_US
dc.subjectgalaxies: ISMen_US
dc.titleMetals and dust content across the galaxies M 101 and NGC 628en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume483
dc.source.issue4
dc.source.beginpage4968-4983
refterms.dateFOA2019-08-05T21:17:10Z


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