SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements
Autor(a) principal: | |
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Data de Publicação: | 2017 |
Outros Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/159745 |
Resumo: | Diffuse ionized gas (DIG) is prevalent in star-forming galaxies. Using a sample of 365 nearly face-on star-forming galaxies observed byMapping 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 Hα regions display enhanced [S II]/Hα, [NII]/Hα, [OII]/Hβ and [O I]/Hα. The gradients in these line ratios are determined by metallicity gradients and Hα. In line ratio diagnostic diagrams, contamination by DIG moves HII 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 HII region models can only shift line ratios slightly relative toHII 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 forDIG with LI(N)ER-like emission. DIG can significantly bias themeasurement 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, R23, 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 HII region models that fail to describe the DIG. |
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Zhang, KaiYan, RenbinBundy, KevinBershady, Matthew A.Haffner, L. MatthewWalterbos, Rene A. M.Maiolino, RobertoTremonti, Christy A.Thomas, D.Drory, NivJones, Amy P.Belfiore, FrancescoSánchez, Sebastián F.Diamond-Stanic, Aleksandar M.Bizyaev, D.Nitschelm, ChristianAndrews, Brett H.Brinkmann, JonBrownstein, Joel R.Cheung, EdmondLi, ChengLaw, David R.Roman-Lopes, AlexandreOravetz, Daniel J.Pan, K.Storchi-Bergmann, ThaisaSimmons, Audrey E.2017-06-20T02:32:29Z20170035-8711http://hdl.handle.net/10183/159745001022481Diffuse ionized gas (DIG) is prevalent in star-forming galaxies. Using a sample of 365 nearly face-on star-forming galaxies observed byMapping 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 Hα regions display enhanced [S II]/Hα, [NII]/Hα, [OII]/Hβ and [O I]/Hα. The gradients in these line ratios are determined by metallicity gradients and Hα. In line ratio diagnostic diagrams, contamination by DIG moves HII 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 HII region models can only shift line ratios slightly relative toHII 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 forDIG with LI(N)ER-like emission. DIG can significantly bias themeasurement 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, R23, 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 HII region models that fail to describe the DIG.application/pdfengMonthly notices of the Royal Astronomical Society. Oxford. Vol. 466, no. 3 (Apr. 2017), p. 3217-3243Galáxias ativasGas ionizadoMetalicidadeFormacao de galaxiasMapeamentos astronômicosGalaxies: abundancesGalaxies: activeGalaxies: evolutionGalaxies: fundamental parametersGalaxies: ISMSDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurementsEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL001022481.pdf001022481.pdfTexto completo (inglês)application/pdf12886246http://www.lume.ufrgs.br/bitstream/10183/159745/1/001022481.pdf5dc2ebea91f7cc3afe8c91094d107162MD51TEXT001022481.pdf.txt001022481.pdf.txtExtracted Texttext/plain113314http://www.lume.ufrgs.br/bitstream/10183/159745/2/001022481.pdf.txt7b6bfdc7bfadd4eb9c6cc6c2988508c4MD52THUMBNAIL001022481.pdf.jpg001022481.pdf.jpgGenerated Thumbnailimage/jpeg2043http://www.lume.ufrgs.br/bitstream/10183/159745/3/001022481.pdf.jpg6039b61aebd0de1b7d227b78521d51a8MD5310183/1597452021-09-18 04:48:56.690925oai:www.lume.ufrgs.br:10183/159745Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2021-09-18T07:48:56Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
title |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
spellingShingle |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements Zhang, Kai Galáxias ativas Gas ionizado Metalicidade Formacao de galaxias Mapeamentos astronômicos Galaxies: abundances Galaxies: active Galaxies: evolution Galaxies: fundamental parameters Galaxies: ISM |
title_short |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
title_full |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
title_fullStr |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
title_full_unstemmed |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
title_sort |
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements |
author |
Zhang, Kai |
author_facet |
Zhang, Kai Yan, Renbin Bundy, Kevin Bershady, Matthew A. Haffner, L. Matthew Walterbos, Rene A. M. Maiolino, Roberto Tremonti, Christy A. Thomas, D. Drory, Niv Jones, Amy P. Belfiore, Francesco Sánchez, Sebastián F. Diamond-Stanic, Aleksandar M. Bizyaev, D. Nitschelm, Christian Andrews, Brett H. Brinkmann, Jon Brownstein, Joel R. Cheung, Edmond Li, Cheng Law, David R. Roman-Lopes, Alexandre Oravetz, Daniel J. Pan, K. Storchi-Bergmann, Thaisa Simmons, Audrey E. |
author_role |
author |
author2 |
Yan, Renbin Bundy, Kevin Bershady, Matthew A. Haffner, L. Matthew Walterbos, Rene A. M. Maiolino, Roberto Tremonti, Christy A. Thomas, D. Drory, Niv Jones, Amy P. Belfiore, Francesco Sánchez, Sebastián F. Diamond-Stanic, Aleksandar M. Bizyaev, D. Nitschelm, Christian Andrews, Brett H. Brinkmann, Jon Brownstein, Joel R. Cheung, Edmond Li, Cheng Law, David R. Roman-Lopes, Alexandre Oravetz, Daniel J. Pan, K. Storchi-Bergmann, Thaisa Simmons, Audrey E. |
author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Zhang, Kai Yan, Renbin Bundy, Kevin Bershady, Matthew A. Haffner, L. Matthew Walterbos, Rene A. M. Maiolino, Roberto Tremonti, Christy A. Thomas, D. Drory, Niv Jones, Amy P. Belfiore, Francesco Sánchez, Sebastián F. Diamond-Stanic, Aleksandar M. Bizyaev, D. Nitschelm, Christian Andrews, Brett H. Brinkmann, Jon Brownstein, Joel R. Cheung, Edmond Li, Cheng Law, David R. Roman-Lopes, Alexandre Oravetz, Daniel J. Pan, K. Storchi-Bergmann, Thaisa Simmons, Audrey E. |
dc.subject.por.fl_str_mv |
Galáxias ativas Gas ionizado Metalicidade Formacao de galaxias Mapeamentos astronômicos |
topic |
Galáxias ativas Gas ionizado Metalicidade Formacao de galaxias Mapeamentos astronômicos Galaxies: abundances Galaxies: active Galaxies: evolution Galaxies: fundamental parameters Galaxies: ISM |
dc.subject.eng.fl_str_mv |
Galaxies: abundances Galaxies: active Galaxies: evolution Galaxies: fundamental parameters Galaxies: ISM |
description |
Diffuse ionized gas (DIG) is prevalent in star-forming galaxies. Using a sample of 365 nearly face-on star-forming galaxies observed byMapping 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 Hα regions display enhanced [S II]/Hα, [NII]/Hα, [OII]/Hβ and [O I]/Hα. The gradients in these line ratios are determined by metallicity gradients and Hα. In line ratio diagnostic diagrams, contamination by DIG moves HII 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 HII region models can only shift line ratios slightly relative toHII 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 forDIG with LI(N)ER-like emission. DIG can significantly bias themeasurement 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, R23, 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 HII region models that fail to describe the DIG. |
publishDate |
2017 |
dc.date.accessioned.fl_str_mv |
2017-06-20T02:32:29Z |
dc.date.issued.fl_str_mv |
2017 |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
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publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/159745 |
dc.identifier.issn.pt_BR.fl_str_mv |
0035-8711 |
dc.identifier.nrb.pt_BR.fl_str_mv |
001022481 |
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0035-8711 001022481 |
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http://hdl.handle.net/10183/159745 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Monthly notices of the Royal Astronomical Society. Oxford. Vol. 466, no. 3 (Apr. 2017), p. 3217-3243 |
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openAccess |
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