The half-mass radius of MaNGA galaxies: effect of IMF gradients

Gradients in the stellar populations (SP) of galaxies – e.g. in age, metallicity, stellar initial mass function (IMF) – can result in gradients in the stellar-mass-to-light ratio, M*/L. Such gradients imply that the distribution of the stellar mass and light is different. For old SPs, e.g. in early-...

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Detalhes bibliográficos
Autores: Bernardi, Mariangela, Sheth, Ravi K., Domínguez Sánchez, Helena, Margalef-Bentabol, Berta, Bizyaev, Dmitry, Lane, Richard R.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/337510
Acesso em linha:http://hdl.handle.net/10261/337510
Access Level:acceso abierto
Palavra-chave:Galaxies: elliptical and lenticular
cD
Galaxies: fundamental parameters
Galaxies: structure
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spelling The half-mass radius of MaNGA galaxies: effect of IMF gradientsBernardi, MariangelaSheth, Ravi K.Domínguez Sánchez, HelenaMargalef-Bentabol, BertaBizyaev, DmitryLane, Richard R.Galaxies: elliptical and lenticularcDGalaxies: fundamental parametersGalaxies: structureGradients in the stellar populations (SP) of galaxies – e.g. in age, metallicity, stellar initial mass function (IMF) – can result in gradients in the stellar-mass-to-light ratio, M*/L. Such gradients imply that the distribution of the stellar mass and light is different. For old SPs, e.g. in early-type galaxies at z ∼ 0, the M*/L gradients are weak if driven by variations in age and metallicity, but significantly larger if driven by the IMF. A gradient which has larger M*/L in the centre increases the estimated total stellar mass (M*) and reduces the scale which contains half this mass (Re,*), compared to when the gradient is ignored. For the IMF gradients inferred from fitting MILES simple SP models to the H β, 〈Fe〉, [MgFe], and TiO2SDSS absorption lines measured in spatially resolved spectra of early-type galaxies in the MaNGA survey, the fractional change in Re,* can be significantly larger than that in M*, especially when the light is more centrally concentrated. The Re,*–M* correlation which results from accounting for IMF gradients is offset to smaller sizes by 0.3 dex compared to when these gradients are ignored. Comparisons with ‘quiescent’ galaxies at higher z must account for evolution in SP gradients (especially age and IMF) and in the light profile before drawing conclusions about how Re,* and M* evolve. The implied merging between higher z and the present is less contrived if Re,*/Re at z ∼ 0 is closer to our IMF-driven gradient calibration than to unity.This work was supported in part by NSF grant AST-1816330. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions.Peer reviewedOxford University PressNational Science Foundation (US)Alfred P. Sloan FoundationDepartment of Energy (US)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/337510reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)InglésThe data underlying this article are available in the Sloan Digital Sky Survey data base at https://www.sdss.org/dr17/https://doi.org/10.1093/mnras/stac3361Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3375102026-05-22T06:33:51Z
dc.title.none.fl_str_mv The half-mass radius of MaNGA galaxies: effect of IMF gradients
title The half-mass radius of MaNGA galaxies: effect of IMF gradients
spellingShingle The half-mass radius of MaNGA galaxies: effect of IMF gradients
Bernardi, Mariangela
Galaxies: elliptical and lenticular
cD
Galaxies: fundamental parameters
Galaxies: structure
title_short The half-mass radius of MaNGA galaxies: effect of IMF gradients
title_full The half-mass radius of MaNGA galaxies: effect of IMF gradients
title_fullStr The half-mass radius of MaNGA galaxies: effect of IMF gradients
title_full_unstemmed The half-mass radius of MaNGA galaxies: effect of IMF gradients
title_sort The half-mass radius of MaNGA galaxies: effect of IMF gradients
dc.creator.none.fl_str_mv Bernardi, Mariangela
Sheth, Ravi K.
Domínguez Sánchez, Helena
Margalef-Bentabol, Berta
Bizyaev, Dmitry
Lane, Richard R.
author Bernardi, Mariangela
author_facet Bernardi, Mariangela
Sheth, Ravi K.
Domínguez Sánchez, Helena
Margalef-Bentabol, Berta
Bizyaev, Dmitry
Lane, Richard R.
author_role author
author2 Sheth, Ravi K.
Domínguez Sánchez, Helena
Margalef-Bentabol, Berta
Bizyaev, Dmitry
Lane, Richard R.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv National Science Foundation (US)
Alfred P. Sloan Foundation
Department of Energy (US)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxies: elliptical and lenticular
cD
Galaxies: fundamental parameters
Galaxies: structure
topic Galaxies: elliptical and lenticular
cD
Galaxies: fundamental parameters
Galaxies: structure
description Gradients in the stellar populations (SP) of galaxies – e.g. in age, metallicity, stellar initial mass function (IMF) – can result in gradients in the stellar-mass-to-light ratio, M*/L. Such gradients imply that the distribution of the stellar mass and light is different. For old SPs, e.g. in early-type galaxies at z ∼ 0, the M*/L gradients are weak if driven by variations in age and metallicity, but significantly larger if driven by the IMF. A gradient which has larger M*/L in the centre increases the estimated total stellar mass (M*) and reduces the scale which contains half this mass (Re,*), compared to when the gradient is ignored. For the IMF gradients inferred from fitting MILES simple SP models to the H β, 〈Fe〉, [MgFe], and TiO2SDSS absorption lines measured in spatially resolved spectra of early-type galaxies in the MaNGA survey, the fractional change in Re,* can be significantly larger than that in M*, especially when the light is more centrally concentrated. The Re,*–M* correlation which results from accounting for IMF gradients is offset to smaller sizes by 0.3 dex compared to when these gradients are ignored. Comparisons with ‘quiescent’ galaxies at higher z must account for evolution in SP gradients (especially age and IMF) and in the light profile before drawing conclusions about how Re,* and M* evolve. The implied merging between higher z and the present is less contrived if Re,*/Re at z ∼ 0 is closer to our IMF-driven gradient calibration than to unity.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/337510
url http://hdl.handle.net/10261/337510
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv The data underlying this article are available in the Sloan Digital Sky Survey data base at https://www.sdss.org/dr17/
https://doi.org/10.1093/mnras/stac3361
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,81155

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