Weak-lensing analysis of galaxy pairs using CS82 data

Autores
Gonzalez, Elizabeth Johana; Rodriguez, Facundo; Garcia Lambas, Diego Rodolfo; Makler, Martín; Mesa, Valeria Alejandra; Alonso, Sol; Duplancic Videla, Maria Fernanda; Pereira, Maria E. S.; Shan, HuanYuan
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Here we analyze a sample of close galaxy pairs (relative projected separation < 25 h -1 kpc and relative radial velocities < 350 km s -1 ) using a weak-lensing analysis based on the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). We determine halo masses for the total sample of pairs as well as for interacting, red, and higher-luminosity pair subsamples with ∼3σ confidence. The derived lensing signal for the total sample can be fitted either by a Singular Isothermal Sphere (SIS) with σ V = 223 ± 24 km s -1 or a Navarro-Frenk-White (NFW) profile with R 200 = 0.30 ± 0.03 h -1 Mpc. The pair total masses and total r band luminosities imply an average mass-to-light ratio of ∼200 h M ⊙ /L ⊙ . On the other hand, red pairs which include a larger fraction of elliptical galaxies, show a larger mass-to-light ratio of ∼345 h M ⊙ /L ⊙ . Derived lensing masses were compared to a proxy of the dynamical mass, obtaining a good correlation. However, there is a large discrepancy between lensing masses and the dynamical mass estimates, which could be accounted for by astrophysical processes such as dynamical friction, by the inclusion of unbound pairs, and by significant deviations of the density distribution from SIS and NFW profiles in the inner regions. We also compared lensing masses with group mass estimates, finding very good agreement with the sample of groups with two members. Red and blue pairs show large differences between group and lensing masses, which is likely due to the single mass-to-light ratio adopted to compute the group masses.
Fil: Gonzalez, Elizabeth Johana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Rodriguez, Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Makler, Martín. Centro Brasileiro de Pesquisas Físicas; Brasil
Fil: Mesa, Valeria Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Provincia de Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Universidad Nacional de Cuyo. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales; Argentina
Fil: Alonso, Sol. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina
Fil: Duplancic Videla, Maria Fernanda. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina
Fil: Pereira, Maria E. S.. Brandeis University; Estados Unidos
Fil: Shan, HuanYuan. Shanghai Astronomical Observatory; República de China
Materia
GALAXIES: GROUPS: GENERAL
GALAXIES: INTERACTIONS
GRAVITATIONAL LENSING: WEAK
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:11336/123778
Acceder
id CONICETDig_aed9f670c47824d6cfff6fdf8b883677
oai_identifier_str oai:ri.conicet.gov.ar:11336/123778
network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Weak-lensing analysis of galaxy pairs using CS82 dataGonzalez, Elizabeth JohanaRodriguez, FacundoGarcia Lambas, Diego RodolfoMakler, MartínMesa, Valeria AlejandraAlonso, SolDuplancic Videla, Maria FernandaPereira, Maria E. S.Shan, HuanYuanGALAXIES: GROUPS: GENERALGALAXIES: INTERACTIONSGRAVITATIONAL LENSING: WEAKhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Here we analyze a sample of close galaxy pairs (relative projected separation < 25 h -1 kpc and relative radial velocities < 350 km s -1 ) using a weak-lensing analysis based on the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). We determine halo masses for the total sample of pairs as well as for interacting, red, and higher-luminosity pair subsamples with ∼3σ confidence. The derived lensing signal for the total sample can be fitted either by a Singular Isothermal Sphere (SIS) with σ V = 223 ± 24 km s -1 or a Navarro-Frenk-White (NFW) profile with R 200 = 0.30 ± 0.03 h -1 Mpc. The pair total masses and total r band luminosities imply an average mass-to-light ratio of ∼200 h M ⊙ /L ⊙ . On the other hand, red pairs which include a larger fraction of elliptical galaxies, show a larger mass-to-light ratio of ∼345 h M ⊙ /L ⊙ . Derived lensing masses were compared to a proxy of the dynamical mass, obtaining a good correlation. However, there is a large discrepancy between lensing masses and the dynamical mass estimates, which could be accounted for by astrophysical processes such as dynamical friction, by the inclusion of unbound pairs, and by significant deviations of the density distribution from SIS and NFW profiles in the inner regions. We also compared lensing masses with group mass estimates, finding very good agreement with the sample of groups with two members. Red and blue pairs show large differences between group and lensing masses, which is likely due to the single mass-to-light ratio adopted to compute the group masses.Fil: Gonzalez, Elizabeth Johana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Rodriguez, Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Makler, Martín. Centro Brasileiro de Pesquisas Físicas; BrasilFil: Mesa, Valeria Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Provincia de Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Universidad Nacional de Cuyo. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales; ArgentinaFil: Alonso, Sol. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; ArgentinaFil: Duplancic Videla, Maria Fernanda. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; ArgentinaFil: Pereira, Maria E. S.. Brandeis University; Estados UnidosFil: Shan, HuanYuan. Shanghai Astronomical Observatory; República de ChinaEDP Sciences2019-01info: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/11336/123778Gonzalez, Elizabeth Johana; Rodriguez, Facundo; Garcia Lambas, Diego Rodolfo; Makler, Martín; Mesa, Valeria Alejandra; et al.; Weak-lensing analysis of galaxy pairs using CS82 data; EDP Sciences; Astronomy and Astrophysics; 621; 1-2019; 1-100004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1811.04940info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2019/01/aa34206-18/aa34206-18.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201834206info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:36:43Zoai:ri.conicet.gov.ar:11336/123778instacron: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:34982025-09-29 09:36:43.896CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Weak-lensing analysis of galaxy pairs using CS82 data
title Weak-lensing analysis of galaxy pairs using CS82 data
spellingShingle Weak-lensing analysis of galaxy pairs using CS82 data
Gonzalez, Elizabeth Johana
GALAXIES: GROUPS: GENERAL
GALAXIES: INTERACTIONS
GRAVITATIONAL LENSING: WEAK
title_short Weak-lensing analysis of galaxy pairs using CS82 data
title_full Weak-lensing analysis of galaxy pairs using CS82 data
title_fullStr Weak-lensing analysis of galaxy pairs using CS82 data
title_full_unstemmed Weak-lensing analysis of galaxy pairs using CS82 data
title_sort Weak-lensing analysis of galaxy pairs using CS82 data
dc.creator.none.fl_str_mv Gonzalez, Elizabeth Johana
Rodriguez, Facundo
Garcia Lambas, Diego Rodolfo
Makler, Martín
Mesa, Valeria Alejandra
Alonso, Sol
Duplancic Videla, Maria Fernanda
Pereira, Maria E. S.
Shan, HuanYuan
author Gonzalez, Elizabeth Johana
author_facet Gonzalez, Elizabeth Johana
Rodriguez, Facundo
Garcia Lambas, Diego Rodolfo
Makler, Martín
Mesa, Valeria Alejandra
Alonso, Sol
Duplancic Videla, Maria Fernanda
Pereira, Maria E. S.
Shan, HuanYuan
author_role author
author2 Rodriguez, Facundo
Garcia Lambas, Diego Rodolfo
Makler, Martín
Mesa, Valeria Alejandra
Alonso, Sol
Duplancic Videla, Maria Fernanda
Pereira, Maria E. S.
Shan, HuanYuan
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: GROUPS: GENERAL
GALAXIES: INTERACTIONS
GRAVITATIONAL LENSING: WEAK
topic GALAXIES: GROUPS: GENERAL
GALAXIES: INTERACTIONS
GRAVITATIONAL LENSING: WEAK
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Here we analyze a sample of close galaxy pairs (relative projected separation < 25 h -1 kpc and relative radial velocities < 350 km s -1 ) using a weak-lensing analysis based on the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). We determine halo masses for the total sample of pairs as well as for interacting, red, and higher-luminosity pair subsamples with ∼3σ confidence. The derived lensing signal for the total sample can be fitted either by a Singular Isothermal Sphere (SIS) with σ V = 223 ± 24 km s -1 or a Navarro-Frenk-White (NFW) profile with R 200 = 0.30 ± 0.03 h -1 Mpc. The pair total masses and total r band luminosities imply an average mass-to-light ratio of ∼200 h M ⊙ /L ⊙ . On the other hand, red pairs which include a larger fraction of elliptical galaxies, show a larger mass-to-light ratio of ∼345 h M ⊙ /L ⊙ . Derived lensing masses were compared to a proxy of the dynamical mass, obtaining a good correlation. However, there is a large discrepancy between lensing masses and the dynamical mass estimates, which could be accounted for by astrophysical processes such as dynamical friction, by the inclusion of unbound pairs, and by significant deviations of the density distribution from SIS and NFW profiles in the inner regions. We also compared lensing masses with group mass estimates, finding very good agreement with the sample of groups with two members. Red and blue pairs show large differences between group and lensing masses, which is likely due to the single mass-to-light ratio adopted to compute the group masses.
Fil: Gonzalez, Elizabeth Johana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Rodriguez, Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Makler, Martín. Centro Brasileiro de Pesquisas Físicas; Brasil
Fil: Mesa, Valeria Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Provincia de Mendoza. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales. Universidad Nacional de Cuyo. Instituto Argentino de Nivología, Glaciología y Ciencias Ambientales; Argentina
Fil: Alonso, Sol. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina
Fil: Duplancic Videla, Maria Fernanda. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina
Fil: Pereira, Maria E. S.. Brandeis University; Estados Unidos
Fil: Shan, HuanYuan. Shanghai Astronomical Observatory; República de China
description Here we analyze a sample of close galaxy pairs (relative projected separation < 25 h -1 kpc and relative radial velocities < 350 km s -1 ) using a weak-lensing analysis based on the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). We determine halo masses for the total sample of pairs as well as for interacting, red, and higher-luminosity pair subsamples with ∼3σ confidence. The derived lensing signal for the total sample can be fitted either by a Singular Isothermal Sphere (SIS) with σ V = 223 ± 24 km s -1 or a Navarro-Frenk-White (NFW) profile with R 200 = 0.30 ± 0.03 h -1 Mpc. The pair total masses and total r band luminosities imply an average mass-to-light ratio of ∼200 h M ⊙ /L ⊙ . On the other hand, red pairs which include a larger fraction of elliptical galaxies, show a larger mass-to-light ratio of ∼345 h M ⊙ /L ⊙ . Derived lensing masses were compared to a proxy of the dynamical mass, obtaining a good correlation. However, there is a large discrepancy between lensing masses and the dynamical mass estimates, which could be accounted for by astrophysical processes such as dynamical friction, by the inclusion of unbound pairs, and by significant deviations of the density distribution from SIS and NFW profiles in the inner regions. We also compared lensing masses with group mass estimates, finding very good agreement with the sample of groups with two members. Red and blue pairs show large differences between group and lensing masses, which is likely due to the single mass-to-light ratio adopted to compute the group masses.
publishDate 2019
dc.date.none.fl_str_mv 2019-01
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/11336/123778
Gonzalez, Elizabeth Johana; Rodriguez, Facundo; Garcia Lambas, Diego Rodolfo; Makler, Martín; Mesa, Valeria Alejandra; et al.; Weak-lensing analysis of galaxy pairs using CS82 data; EDP Sciences; Astronomy and Astrophysics; 621; 1-2019; 1-10
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/123778
identifier_str_mv Gonzalez, Elizabeth Johana; Rodriguez, Facundo; Garcia Lambas, Diego Rodolfo; Makler, Martín; Mesa, Valeria Alejandra; et al.; Weak-lensing analysis of galaxy pairs using CS82 data; EDP Sciences; Astronomy and Astrophysics; 621; 1-2019; 1-10
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1811.04940
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2019/01/aa34206-18/aa34206-18.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201834206
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 EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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 13.070432

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