Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey

Autores
Cano Díaz, M.; Sánchez, S. F.; Zibetti, S.; Ascasibar, Y.; Bland Hawthorn, J.; Ziegler, B.; González Delgado, R. M.; Walcher, C.J.; García Benito, Rubén; Mast, Damian; Mendoza Pérez, M. A.; Falcón Barroso, J.; Galbany, Lluís; Husemann, Bernd; Kehrig, C.; Marino, R. A.; Sánchez Blázquez, P.; López Cobá, C.; López Sánchez, Á. R.; Vílchez, J. M.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The "main sequence of galaxies" - defined in terms of the total star formation rate ψ versus the total stellar mass M ∗ - is a well-studied tight relation that has been observed at several wavelengths and at different redshifts. All earlier studies have derived this relation from integrated properties of galaxies. We recover the same relation from an analysis of spatially resolved properties, with integral field spectroscopic (IFS) observations of 306 galaxies from the CALIFA survey. We consider the SFR surface density in units of log(M o yr-1 Kpc-2) and the stellar mass surface density in units of log(M o Kpc-2) in individual spaxels that probe spatial scales of 0.5-1.5 Kpc. This local relation exhibits a high degree of correlation with small scatter (σ = 0.23 dex), irrespective of the dominant ionization source of the host galaxy or its integrated stellar mass. We highlight (i) the integrated star formation main sequence formed by galaxies whose dominant ionization process is related to star formation, for which we find a slope of 0.81 ± 0.02; (ii) for the spatially resolved relation obtained with the spaxel analysis, we find a slope of 0.72 ± 0.04; and (iii) for the integrated main sequence, we also identified a sequence formed by galaxies that are dominated by an old stellar population, which we have called the retired galaxies sequence.
Fil: Cano Díaz, M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Sánchez, S. F.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Zibetti, S.. Osservatorio Astrofisico di Arcetri; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Ascasibar, Y.. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; España
Fil: Bland Hawthorn, J.. University of Sydney; Australia
Fil: Ziegler, B.. Universidad de Viena; Austria
Fil: González Delgado, R. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Walcher, C.J.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: García Benito, Rubén. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Mast, Damian. 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
Fil: Mendoza Pérez, M. A.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Falcón Barroso, J.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
Fil: Galbany, Lluís. Millennium Institute of Astrophysics; Chile. Universidad de Chile; Chile
Fil: Husemann, Bernd. European Southern Observator; Alemania
Fil: Kehrig, C.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Marino, R. A.. Universidad Complutense de Madrid; España. ETH Zurich’s Institute for Astronomy; Alemania
Fil: Sánchez Blázquez, P.. Universidad Autónoma de Madrid; España. Pontificia Universidad Católica de Chile; Chile
Fil: López Cobá, C.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: López Sánchez, Á. R.. Australian Astronomical Observatory; Australia. Macquarie University; Australia
Fil: Vílchez, J. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Materia
GALAXIES: EVOLUTION
GALAXIES: FUNDAMENTAL PARAMETERS
GALAXIES: STAR FORMATION
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/180444
Acceder
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spelling Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa SurveyCano Díaz, M.Sánchez, S. F.Zibetti, S.Ascasibar, Y.Bland Hawthorn, J.Ziegler, B.González Delgado, R. M.Walcher, C.J.García Benito, RubénMast, DamianMendoza Pérez, M. A.Falcón Barroso, J.Galbany, LluísHusemann, BerndKehrig, C.Marino, R. A.Sánchez Blázquez, P.López Cobá, C.López Sánchez, Á. R.Vílchez, J. M.GALAXIES: EVOLUTIONGALAXIES: FUNDAMENTAL PARAMETERSGALAXIES: STAR FORMATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The "main sequence of galaxies" - defined in terms of the total star formation rate ψ versus the total stellar mass M ∗ - is a well-studied tight relation that has been observed at several wavelengths and at different redshifts. All earlier studies have derived this relation from integrated properties of galaxies. We recover the same relation from an analysis of spatially resolved properties, with integral field spectroscopic (IFS) observations of 306 galaxies from the CALIFA survey. We consider the SFR surface density in units of log(M o yr-1 Kpc-2) and the stellar mass surface density in units of log(M o Kpc-2) in individual spaxels that probe spatial scales of 0.5-1.5 Kpc. This local relation exhibits a high degree of correlation with small scatter (σ = 0.23 dex), irrespective of the dominant ionization source of the host galaxy or its integrated stellar mass. We highlight (i) the integrated star formation main sequence formed by galaxies whose dominant ionization process is related to star formation, for which we find a slope of 0.81 ± 0.02; (ii) for the spatially resolved relation obtained with the spaxel analysis, we find a slope of 0.72 ± 0.04; and (iii) for the integrated main sequence, we also identified a sequence formed by galaxies that are dominated by an old stellar population, which we have called the retired galaxies sequence.Fil: Cano Díaz, M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: Sánchez, S. F.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: Zibetti, S.. Osservatorio Astrofisico di Arcetri; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Ascasibar, Y.. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Bland Hawthorn, J.. University of Sydney; AustraliaFil: Ziegler, B.. Universidad de Viena; AustriaFil: González Delgado, R. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Walcher, C.J.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: García Benito, Rubén. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Mast, Damian. 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; ArgentinaFil: Mendoza Pérez, M. A.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Falcón Barroso, J.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; EspañaFil: Galbany, Lluís. Millennium Institute of Astrophysics; Chile. Universidad de Chile; ChileFil: Husemann, Bernd. European Southern Observator; AlemaniaFil: Kehrig, C.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Marino, R. A.. Universidad Complutense de Madrid; España. ETH Zurich’s Institute for Astronomy; AlemaniaFil: Sánchez Blázquez, P.. Universidad Autónoma de Madrid; España. Pontificia Universidad Católica de Chile; ChileFil: López Cobá, C.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: López Sánchez, Á. R.. Australian Astronomical Observatory; Australia. Macquarie University; AustraliaFil: Vílchez, J. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaIOP Publishing2016-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/180444Cano Díaz, M.; Sánchez, S. F.; Zibetti, S.; Ascasibar, Y.; Bland Hawthorn, J.; et al.; Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey; IOP Publishing; Astrophysical Journal; 821; 2; 4-2016; 1-50004-637X1538-4357CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/2041-8205/821/2/L26info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8205/821/2/L26info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1602.02770info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:17:39Zoai:ri.conicet.gov.ar:11336/180444instacron: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:34982025-10-22 11:17:39.495CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
title Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
spellingShingle Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
Cano Díaz, M.
GALAXIES: EVOLUTION
GALAXIES: FUNDAMENTAL PARAMETERS
GALAXIES: STAR FORMATION
title_short Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
title_full Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
title_fullStr Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
title_full_unstemmed Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
title_sort Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey
dc.creator.none.fl_str_mv Cano Díaz, M.
Sánchez, S. F.
Zibetti, S.
Ascasibar, Y.
Bland Hawthorn, J.
Ziegler, B.
González Delgado, R. M.
Walcher, C.J.
García Benito, Rubén
Mast, Damian
Mendoza Pérez, M. A.
Falcón Barroso, J.
Galbany, Lluís
Husemann, Bernd
Kehrig, C.
Marino, R. A.
Sánchez Blázquez, P.
López Cobá, C.
López Sánchez, Á. R.
Vílchez, J. M.
author Cano Díaz, M.
author_facet Cano Díaz, M.
Sánchez, S. F.
Zibetti, S.
Ascasibar, Y.
Bland Hawthorn, J.
Ziegler, B.
González Delgado, R. M.
Walcher, C.J.
García Benito, Rubén
Mast, Damian
Mendoza Pérez, M. A.
Falcón Barroso, J.
Galbany, Lluís
Husemann, Bernd
Kehrig, C.
Marino, R. A.
Sánchez Blázquez, P.
López Cobá, C.
López Sánchez, Á. R.
Vílchez, J. M.
author_role author
author2 Sánchez, S. F.
Zibetti, S.
Ascasibar, Y.
Bland Hawthorn, J.
Ziegler, B.
González Delgado, R. M.
Walcher, C.J.
García Benito, Rubén
Mast, Damian
Mendoza Pérez, M. A.
Falcón Barroso, J.
Galbany, Lluís
Husemann, Bernd
Kehrig, C.
Marino, R. A.
Sánchez Blázquez, P.
López Cobá, C.
López Sánchez, Á. R.
Vílchez, J. M.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: EVOLUTION
GALAXIES: FUNDAMENTAL PARAMETERS
GALAXIES: STAR FORMATION
topic GALAXIES: EVOLUTION
GALAXIES: FUNDAMENTAL PARAMETERS
GALAXIES: STAR FORMATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The "main sequence of galaxies" - defined in terms of the total star formation rate ψ versus the total stellar mass M ∗ - is a well-studied tight relation that has been observed at several wavelengths and at different redshifts. All earlier studies have derived this relation from integrated properties of galaxies. We recover the same relation from an analysis of spatially resolved properties, with integral field spectroscopic (IFS) observations of 306 galaxies from the CALIFA survey. We consider the SFR surface density in units of log(M o yr-1 Kpc-2) and the stellar mass surface density in units of log(M o Kpc-2) in individual spaxels that probe spatial scales of 0.5-1.5 Kpc. This local relation exhibits a high degree of correlation with small scatter (σ = 0.23 dex), irrespective of the dominant ionization source of the host galaxy or its integrated stellar mass. We highlight (i) the integrated star formation main sequence formed by galaxies whose dominant ionization process is related to star formation, for which we find a slope of 0.81 ± 0.02; (ii) for the spatially resolved relation obtained with the spaxel analysis, we find a slope of 0.72 ± 0.04; and (iii) for the integrated main sequence, we also identified a sequence formed by galaxies that are dominated by an old stellar population, which we have called the retired galaxies sequence.
Fil: Cano Díaz, M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Sánchez, S. F.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Zibetti, S.. Osservatorio Astrofisico di Arcetri; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Ascasibar, Y.. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; España
Fil: Bland Hawthorn, J.. University of Sydney; Australia
Fil: Ziegler, B.. Universidad de Viena; Austria
Fil: González Delgado, R. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Walcher, C.J.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: García Benito, Rubén. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Mast, Damian. 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
Fil: Mendoza Pérez, M. A.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Falcón Barroso, J.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
Fil: Galbany, Lluís. Millennium Institute of Astrophysics; Chile. Universidad de Chile; Chile
Fil: Husemann, Bernd. European Southern Observator; Alemania
Fil: Kehrig, C.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Marino, R. A.. Universidad Complutense de Madrid; España. ETH Zurich’s Institute for Astronomy; Alemania
Fil: Sánchez Blázquez, P.. Universidad Autónoma de Madrid; España. Pontificia Universidad Católica de Chile; Chile
Fil: López Cobá, C.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: López Sánchez, Á. R.. Australian Astronomical Observatory; Australia. Macquarie University; Australia
Fil: Vílchez, J. M.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
description The "main sequence of galaxies" - defined in terms of the total star formation rate ψ versus the total stellar mass M ∗ - is a well-studied tight relation that has been observed at several wavelengths and at different redshifts. All earlier studies have derived this relation from integrated properties of galaxies. We recover the same relation from an analysis of spatially resolved properties, with integral field spectroscopic (IFS) observations of 306 galaxies from the CALIFA survey. We consider the SFR surface density in units of log(M o yr-1 Kpc-2) and the stellar mass surface density in units of log(M o Kpc-2) in individual spaxels that probe spatial scales of 0.5-1.5 Kpc. This local relation exhibits a high degree of correlation with small scatter (σ = 0.23 dex), irrespective of the dominant ionization source of the host galaxy or its integrated stellar mass. We highlight (i) the integrated star formation main sequence formed by galaxies whose dominant ionization process is related to star formation, for which we find a slope of 0.81 ± 0.02; (ii) for the spatially resolved relation obtained with the spaxel analysis, we find a slope of 0.72 ± 0.04; and (iii) for the integrated main sequence, we also identified a sequence formed by galaxies that are dominated by an old stellar population, which we have called the retired galaxies sequence.
publishDate 2016
dc.date.none.fl_str_mv 2016-04
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/11336/180444
Cano Díaz, M.; Sánchez, S. F.; Zibetti, S.; Ascasibar, Y.; Bland Hawthorn, J.; et al.; Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey; IOP Publishing; Astrophysical Journal; 821; 2; 4-2016; 1-5
0004-637X
1538-4357
CONICET Digital
CONICET
url http://hdl.handle.net/11336/180444
identifier_str_mv Cano Díaz, M.; Sánchez, S. F.; Zibetti, S.; Ascasibar, Y.; Bland Hawthorn, J.; et al.; Spatially Resolved Star Formation Main Sequence of Galaxies in the Califa Survey; IOP Publishing; Astrophysical Journal; 821; 2; 4-2016; 1-5
0004-637X
1538-4357
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://iopscience.iop.org/article/10.3847/2041-8205/821/2/L26
info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8205/821/2/L26
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1602.02770
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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