The mass-metallicity relation of interacting galaxies

Autores
Michel-Dansac, Leopold; Garcia Lambas, Diego Rodolfo; Alonso Giraldes, Maria Sol; Tissera, Patricia Beatriz
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We study the mass–metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h−1 and radial velocity V < 350 km s−1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass–metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M∗ 109 M h−1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M∗ 1010 M h−1) galaxies have a systematically lower metallicity, although with a smaller difference (−0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings.
Fil: Michel-Dansac, Leopold. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Alonso Giraldes, Maria Sol. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito"; Argentina
Fil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Materia
galaxy:evolution
galaxy:formation
galaxy.abundances
galaxy:interactions
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/24692
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/24692
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The mass-metallicity relation of interacting galaxiesMichel-Dansac, LeopoldGarcia Lambas, Diego RodolfoAlonso Giraldes, Maria SolTissera, Patricia Beatrizgalaxy:evolutiongalaxy:formationgalaxy.abundancesgalaxy:interactionshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We study the mass–metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h−1 and radial velocity V < 350 km s−1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass–metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M∗ 109 M h−1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M∗ 1010 M h−1) galaxies have a systematically lower metallicity, although with a smaller difference (−0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings.Fil: Michel-Dansac, Leopold. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Alonso Giraldes, Maria Sol. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito"; ArgentinaFil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaOxford University Press2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/24692Michel-Dansac, Leopold; Garcia Lambas, Diego Rodolfo; Alonso Giraldes, Maria Sol; Tissera, Patricia Beatriz; The mass-metallicity relation of interacting galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 386; 1; 12-2008; 82-860035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1745-3933.2008.00466.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnrasl/article-lookup/doi/10.1111/j.1745-3933.2008.00466.xinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:51:14Zoai:ri.conicet.gov.ar:11336/24692instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-03 09:51:14.562CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The mass-metallicity relation of interacting galaxies
title The mass-metallicity relation of interacting galaxies
spellingShingle The mass-metallicity relation of interacting galaxies
Michel-Dansac, Leopold
galaxy:evolution
galaxy:formation
galaxy.abundances
galaxy:interactions
title_short The mass-metallicity relation of interacting galaxies
title_full The mass-metallicity relation of interacting galaxies
title_fullStr The mass-metallicity relation of interacting galaxies
title_full_unstemmed The mass-metallicity relation of interacting galaxies
title_sort The mass-metallicity relation of interacting galaxies
dc.creator.none.fl_str_mv Michel-Dansac, Leopold
Garcia Lambas, Diego Rodolfo
Alonso Giraldes, Maria Sol
Tissera, Patricia Beatriz
author Michel-Dansac, Leopold
author_facet Michel-Dansac, Leopold
Garcia Lambas, Diego Rodolfo
Alonso Giraldes, Maria Sol
Tissera, Patricia Beatriz
author_role author
author2 Garcia Lambas, Diego Rodolfo
Alonso Giraldes, Maria Sol
Tissera, Patricia Beatriz
author2_role author
author
author
dc.subject.none.fl_str_mv galaxy:evolution
galaxy:formation
galaxy.abundances
galaxy:interactions
topic galaxy:evolution
galaxy:formation
galaxy.abundances
galaxy:interactions
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We study the mass–metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h−1 and radial velocity V < 350 km s−1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass–metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M∗ 109 M h−1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M∗ 1010 M h−1) galaxies have a systematically lower metallicity, although with a smaller difference (−0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings.
Fil: Michel-Dansac, Leopold. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; Argentina
Fil: Alonso Giraldes, Maria Sol. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito"; Argentina
Fil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
description We study the mass–metallicity relation of galaxies in pairs and in isolation taken from the Sloan Digital Sky Survey-Data Release 4 (SDSS-DR4) using the stellar masses and oxygen abundances derived by Tremonti et al. Close galaxy pairs, defined by projected separation rp < 25 kpc h−1 and radial velocity V < 350 km s−1, are morphologically classified according to the strength of the interaction signs. We find that only for pairs showing signs of strong interactions, the mass–metallicity relation differs significantly from that of galaxies in isolation. In such pairs, the mean gas-phase oxygen abundances of galaxies with low stellar masses (M∗ 109 M h−1) exhibit an excess of 0.2 dex. Conversely, at larger masses (M∗ 1010 M h−1) galaxies have a systematically lower metallicity, although with a smaller difference (−0.05 dex). Similar trends are obtained if g-band magnitudes are used instead of stellar masses. In minor interactions, we find that the less massive member is systematically enriched, while a galaxy in interaction with a comparable stellar mass companion shows a metallicity decrement with respect to galaxies in isolation. We argue that metal-rich starbursts triggered by a more massive component, and inflows of low-metallicity gas induced by comparable or less massive companion galaxies, provide a natural scenario to explain our findings.
publishDate 2008
dc.date.none.fl_str_mv 2008-12
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/24692
Michel-Dansac, Leopold; Garcia Lambas, Diego Rodolfo; Alonso Giraldes, Maria Sol; Tissera, Patricia Beatriz; The mass-metallicity relation of interacting galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 386; 1; 12-2008; 82-86
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/24692
identifier_str_mv Michel-Dansac, Leopold; Garcia Lambas, Diego Rodolfo; Alonso Giraldes, Maria Sol; Tissera, Patricia Beatriz; The mass-metallicity relation of interacting galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 386; 1; 12-2008; 82-86
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1745-3933.2008.00466.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnrasl/article-lookup/doi/10.1111/j.1745-3933.2008.00466.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
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:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.13397

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