SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/196017 |
Resumo: | The large Integral Field Spectroscopy surveys have allowed the classification of ionizing sources of emission lines on sub-kiloparsec scales. In this work, we define two non-parametric parameters, quiescence (Fq) and its concentration (Cq), to quantify the strength and the spatial distribution of the quenched areas, respectively, traced by the LI(N)ER regions with low EW(Hα). With these two measurements, we classify MaNGA galaxies into inside-out and outside-in quenching types according to their locations on the Fqversus Cqplane and we measure the fraction of inside-out (outside-in) quenching galaxies as a function of halo mass. We find that the fraction of galaxies showing inside-out quenching increases with halo mass, irrespective of stellar mass or galaxy type (satellites versus centrals). In addition, high-stellar-mass galaxies exhibit a greater fraction of inside-out quenching compared to low-stellar-mass ones in all environments. In contrast, the fraction of outside-in quenching does not depend on halo mass. Our results suggest that morphological quenching may be responsible for the inside-out quenching seen in all environments. On the other hand, the flat dependence of the outside-in quenching on halo mass could be a mixed result of ram pressure stripping and galaxy mergers. Nevertheless, for a given environment and stellar mass, the fraction of inside-out quenching is systematically greater than that of outside-in quenching, suggesting that inside-out quenching is the dominant quenching mode in all environments. |
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Lin, LihwaiHsieh, BauchingPan, Hsi AnRembold, Sandro BarbozaSánchez, Sebastián F.Argudo-Fernández, MariaRowlands, KateBelfiore, FrancescoBizyaev, D.Lacerna, IvanRiffel, RogérioRong, YuYuan, FangDrory, NivMaiolino, RobertoWilcots, Eric2019-06-20T02:36:06Z20190004-637Xhttp://hdl.handle.net/10183/196017001095707The large Integral Field Spectroscopy surveys have allowed the classification of ionizing sources of emission lines on sub-kiloparsec scales. In this work, we define two non-parametric parameters, quiescence (Fq) and its concentration (Cq), to quantify the strength and the spatial distribution of the quenched areas, respectively, traced by the LI(N)ER regions with low EW(Hα). With these two measurements, we classify MaNGA galaxies into inside-out and outside-in quenching types according to their locations on the Fqversus Cqplane and we measure the fraction of inside-out (outside-in) quenching galaxies as a function of halo mass. We find that the fraction of galaxies showing inside-out quenching increases with halo mass, irrespective of stellar mass or galaxy type (satellites versus centrals). In addition, high-stellar-mass galaxies exhibit a greater fraction of inside-out quenching compared to low-stellar-mass ones in all environments. In contrast, the fraction of outside-in quenching does not depend on halo mass. Our results suggest that morphological quenching may be responsible for the inside-out quenching seen in all environments. On the other hand, the flat dependence of the outside-in quenching on halo mass could be a mixed result of ram pressure stripping and galaxy mergers. Nevertheless, for a given environment and stellar mass, the fraction of inside-out quenching is systematically greater than that of outside-in quenching, suggesting that inside-out quenching is the dominant quenching mode in all environments.application/pdfengThe astrophysical journal. Bristol. Vol. 872, no. 1 (Feb. 2019), 50, 14 p.HalosGaláxiasEvolucao galaticaGalaxies: evolutionGalaxies: generalGalaxies: star formationSDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environmentsEstrangeiroinfo: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:UFRGSTEXT001095707.pdf.txt001095707.pdf.txtExtracted Texttext/plain69920http://www.lume.ufrgs.br/bitstream/10183/196017/2/001095707.pdf.txt9bcf764a5a782d91419e7304241d1b49MD52ORIGINAL001095707.pdfTexto completo (inglês)application/pdf5608804http://www.lume.ufrgs.br/bitstream/10183/196017/1/001095707.pdf85a41ef51b2e34b49d5d9438c1bac627MD5110183/1960172023-09-24 03:40:01.185543oai:www.lume.ufrgs.br:10183/196017Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-09-24T06:40:01Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
title |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
spellingShingle |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments Lin, Lihwai Halos Galáxias Evolucao galatica Galaxies: evolution Galaxies: general Galaxies: star formation |
title_short |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
title_full |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
title_fullStr |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
title_full_unstemmed |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
title_sort |
SDSS-IV MaNGA : inside-out versus outside-in quenching of galaxies in different local environments |
author |
Lin, Lihwai |
author_facet |
Lin, Lihwai Hsieh, Bauching Pan, Hsi An Rembold, Sandro Barboza Sánchez, Sebastián F. Argudo-Fernández, Maria Rowlands, Kate Belfiore, Francesco Bizyaev, D. Lacerna, Ivan Riffel, Rogério Rong, Yu Yuan, Fang Drory, Niv Maiolino, Roberto Wilcots, Eric |
author_role |
author |
author2 |
Hsieh, Bauching Pan, Hsi An Rembold, Sandro Barboza Sánchez, Sebastián F. Argudo-Fernández, Maria Rowlands, Kate Belfiore, Francesco Bizyaev, D. Lacerna, Ivan Riffel, Rogério Rong, Yu Yuan, Fang Drory, Niv Maiolino, Roberto Wilcots, Eric |
author2_role |
author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Lin, Lihwai Hsieh, Bauching Pan, Hsi An Rembold, Sandro Barboza Sánchez, Sebastián F. Argudo-Fernández, Maria Rowlands, Kate Belfiore, Francesco Bizyaev, D. Lacerna, Ivan Riffel, Rogério Rong, Yu Yuan, Fang Drory, Niv Maiolino, Roberto Wilcots, Eric |
dc.subject.por.fl_str_mv |
Halos Galáxias Evolucao galatica |
topic |
Halos Galáxias Evolucao galatica Galaxies: evolution Galaxies: general Galaxies: star formation |
dc.subject.eng.fl_str_mv |
Galaxies: evolution Galaxies: general Galaxies: star formation |
description |
The large Integral Field Spectroscopy surveys have allowed the classification of ionizing sources of emission lines on sub-kiloparsec scales. In this work, we define two non-parametric parameters, quiescence (Fq) and its concentration (Cq), to quantify the strength and the spatial distribution of the quenched areas, respectively, traced by the LI(N)ER regions with low EW(Hα). With these two measurements, we classify MaNGA galaxies into inside-out and outside-in quenching types according to their locations on the Fqversus Cqplane and we measure the fraction of inside-out (outside-in) quenching galaxies as a function of halo mass. We find that the fraction of galaxies showing inside-out quenching increases with halo mass, irrespective of stellar mass or galaxy type (satellites versus centrals). In addition, high-stellar-mass galaxies exhibit a greater fraction of inside-out quenching compared to low-stellar-mass ones in all environments. In contrast, the fraction of outside-in quenching does not depend on halo mass. Our results suggest that morphological quenching may be responsible for the inside-out quenching seen in all environments. On the other hand, the flat dependence of the outside-in quenching on halo mass could be a mixed result of ram pressure stripping and galaxy mergers. Nevertheless, for a given environment and stellar mass, the fraction of inside-out quenching is systematically greater than that of outside-in quenching, suggesting that inside-out quenching is the dominant quenching mode in all environments. |
publishDate |
2019 |
dc.date.accessioned.fl_str_mv |
2019-06-20T02:36:06Z |
dc.date.issued.fl_str_mv |
2019 |
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 |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/196017 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
001095707 |
identifier_str_mv |
0004-637X 001095707 |
url |
http://hdl.handle.net/10183/196017 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Bristol. Vol. 872, no. 1 (Feb. 2019), 50, 14 p. |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
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UFRGS |
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Repositório Institucional da UFRGS |
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Repositório Institucional da UFRGS |
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http://www.lume.ufrgs.br/bitstream/10183/196017/2/001095707.pdf.txt http://www.lume.ufrgs.br/bitstream/10183/196017/1/001095707.pdf |
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