Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29762
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Zhang, Kai | en_US |
dc.contributor.author | Yan, Renbin | en_US |
dc.contributor.author | Bundy, Kevin | en_US |
dc.contributor.author | Bershady, Matthew | en_US |
dc.contributor.author | Haffner, L. Matthew | en_US |
dc.contributor.author | Walterbos, René | en_US |
dc.contributor.author | Maiolino, Roberto | en_US |
dc.contributor.author | Tremonti, Christy | en_US |
dc.contributor.author | Thomas, Daniel | en_US |
dc.contributor.author | Drory, Niv | en_US |
dc.contributor.author | Jones, Amy | en_US |
dc.contributor.author | BELFIORE, FRANCESCO MICHEL CONCETTO | en_US |
dc.contributor.author | Sánchez, Sebastian F. | en_US |
dc.contributor.author | Diamond-Stanic, Aleksandar M. | en_US |
dc.contributor.author | Bizyaev, Dmitry | en_US |
dc.contributor.author | Nitschelm, Christian | en_US |
dc.contributor.author | Andrews, Brett | en_US |
dc.contributor.author | Brinkmann, Jon | en_US |
dc.contributor.author | Brownstein, Joel R. | en_US |
dc.contributor.author | Cheung, Edmond | en_US |
dc.contributor.author | Li, Cheng | en_US |
dc.contributor.author | Law, David R. | en_US |
dc.contributor.author | Roman Lopes, Alexandre | en_US |
dc.contributor.author | Oravetz, Daniel | en_US |
dc.contributor.author | Pan, Kaike | en_US |
dc.contributor.author | Storchi Bergmann, Thaisa | en_US |
dc.contributor.author | Simmons, Audrey | en_US |
dc.date.accessioned | 2021-01-13T17:13:24Z | - |
dc.date.available | 2021-01-13T17:13:24Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29762 | - |
dc.description.abstract | Diffuse ionized gas (DIG) is prevalent in star-forming galaxies. Using a sample of 365 nearly face-on star-forming galaxies observed by Mapping Nearby Galaxies at APO, we demonstrate how DIG in star-forming galaxies impacts the measurements of emission-line ratios, hence the interpretation of diagnostic diagrams and gas-phase metallicity measurements. At fixed metallicity, DIG-dominated low Σ<SUB>Hα</SUB> regions display enhanced [S II]/Hα, [N II]/Hα, [O II]/Hβ and [O I]/Hα. The gradients in these line ratios are determined by metallicity gradients and Σ<SUB>Hα</SUB>. In line ratio diagnostic diagrams, contamination by DIG moves H II regions towards composite or low-ionization nuclear emission-line region (LI(N)ER)-like regions. A harder ionizing spectrum is needed to explain DIG line ratios. Leaky H II region models can only shift line ratios slightly relative to H II region models, and thus fail to explain the composite/LI(N)ER line ratios displayed by DIG. Our result favours ionization by evolved stars as a major ionization source for DIG with LI(N)ER-like emission. DIG can significantly bias the measurement of gas metallicity and metallicity gradients derived using strong-line methods. Metallicities derived using N2O2 are optimal because they exhibit the smallest bias and error. Using O3N2, R<SUB>23</SUB>, N2 = [N II]/Hα and N2S2Hα to derive metallicities introduces bias in the derived metallicity gradients as large as the gradient itself. The strong-line method of Blanc et al. (IZI hereafter) cannot be applied to DIG to get an accurate metallicity because it currently contains only H II region models that fail to describe the DIG. | en_US |
dc.language.iso | eng | en_US |
dc.title | SDSS-IV MaNGA: the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw3308 | en_US |
dc.identifier.scopus | 2-s2.0-85018285808 | en_US |
dc.identifier.isi | 000398418600050 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/466/3/3217/2726592 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 466 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3217 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017MNRAS.466.3217Z | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | 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.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0002-2545-5752 | - |
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