Mapping the galaxy NGC 4486 (M87) through its globular cluster system
- Autores
- Forte, Juan Carlos; Vega, Ema Irene; Faifer, Favio Raúl
- Año de publicación
- 2012
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- As shown in previous works, globular clusters (GCs) can be used to trace the overall structure of the diffuse stellar populations in early-type galaxies if the number of clusters per unit stellar mass depends on metallicity. In this paper we further test this assumption in the galaxy NGC 4486 (M87) by combining several data sources. The results show that GCs allow the mapping of the galaxy in terms of the surface brightness profile, integrated colour gradient, chemical abundance and mass-to-luminosity ratios up to 1000arcsec (or 80.4kpc) from its centre (i.e. some 10 effective radii). The analysis indicates the presence of a dominant high-metallicity bulge associated with the red globulars, whose ellipticity increases outwards, and of a more flattened low-metallicity halo connected with the blue globulars. The chemical abundance gradient of the composite stellar population is remarkably similar to that inferred from X-ray observations of hot gas. The mass-metallicity spectrum of the stellar population can, in principle, be understood in terms of inhomogeneous enrichment models. In turn, the distribution of the bluest GCs, and lowest metallicity halo stars, has an intriguing similarity with that of dark matter, a feature shared with NGC 1399. Also, in these two galaxies, the number of blue GCs per dark mass unit is identical within the errors, ≈1.0(±0.3) × 10-9. The total stellar mass derived for NGC 4486 is 6.8(±1.1) × 1011 M⊙ with a baryonic mass fraction fb= 0.08(±0.01).
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Galaxies: haloes
Galaxies: star clusters: general
Globular clusters: general - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84681
Ver los metadatos del registro completo
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Mapping the galaxy NGC 4486 (M87) through its globular cluster systemForte, Juan CarlosVega, Ema IreneFaifer, Favio RaúlCiencias AstronómicasGalaxies: haloesGalaxies: star clusters: generalGlobular clusters: generalAs shown in previous works, globular clusters (GCs) can be used to trace the overall structure of the diffuse stellar populations in early-type galaxies if the number of clusters per unit stellar mass depends on metallicity. In this paper we further test this assumption in the galaxy NGC 4486 (M87) by combining several data sources. The results show that GCs allow the mapping of the galaxy in terms of the surface brightness profile, integrated colour gradient, chemical abundance and mass-to-luminosity ratios up to 1000arcsec (or 80.4kpc) from its centre (i.e. some 10 effective radii). The analysis indicates the presence of a dominant high-metallicity bulge associated with the red globulars, whose ellipticity increases outwards, and of a more flattened low-metallicity halo connected with the blue globulars. The chemical abundance gradient of the composite stellar population is remarkably similar to that inferred from X-ray observations of hot gas. The mass-metallicity spectrum of the stellar population can, in principle, be understood in terms of inhomogeneous enrichment models. In turn, the distribution of the bluest GCs, and lowest metallicity halo stars, has an intriguing similarity with that of dark matter, a feature shared with NGC 1399. Also, in these two galaxies, the number of blue GCs per dark mass unit is identical within the errors, ≈1.0(±0.3) × 10<SUP>-9</SUP>. The total stellar mass derived for NGC 4486 is 6.8(±1.1) × 10<SUP>11</SUP> M⊙ with a baryonic mass fraction f<SUB>b</SUB>= 0.08(±0.01).Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2012info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf635-650http://sedici.unlp.edu.ar/handle/10915/84681enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.20341.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:05Zoai:sedici.unlp.edu.ar:10915/84681Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:05.46SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
title |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
spellingShingle |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system Forte, Juan Carlos Ciencias Astronómicas Galaxies: haloes Galaxies: star clusters: general Globular clusters: general |
title_short |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
title_full |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
title_fullStr |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
title_full_unstemmed |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
title_sort |
Mapping the galaxy NGC 4486 (M87) through its globular cluster system |
dc.creator.none.fl_str_mv |
Forte, Juan Carlos Vega, Ema Irene Faifer, Favio Raúl |
author |
Forte, Juan Carlos |
author_facet |
Forte, Juan Carlos Vega, Ema Irene Faifer, Favio Raúl |
author_role |
author |
author2 |
Vega, Ema Irene Faifer, Favio Raúl |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Galaxies: haloes Galaxies: star clusters: general Globular clusters: general |
topic |
Ciencias Astronómicas Galaxies: haloes Galaxies: star clusters: general Globular clusters: general |
dc.description.none.fl_txt_mv |
As shown in previous works, globular clusters (GCs) can be used to trace the overall structure of the diffuse stellar populations in early-type galaxies if the number of clusters per unit stellar mass depends on metallicity. In this paper we further test this assumption in the galaxy NGC 4486 (M87) by combining several data sources. The results show that GCs allow the mapping of the galaxy in terms of the surface brightness profile, integrated colour gradient, chemical abundance and mass-to-luminosity ratios up to 1000arcsec (or 80.4kpc) from its centre (i.e. some 10 effective radii). The analysis indicates the presence of a dominant high-metallicity bulge associated with the red globulars, whose ellipticity increases outwards, and of a more flattened low-metallicity halo connected with the blue globulars. The chemical abundance gradient of the composite stellar population is remarkably similar to that inferred from X-ray observations of hot gas. The mass-metallicity spectrum of the stellar population can, in principle, be understood in terms of inhomogeneous enrichment models. In turn, the distribution of the bluest GCs, and lowest metallicity halo stars, has an intriguing similarity with that of dark matter, a feature shared with NGC 1399. Also, in these two galaxies, the number of blue GCs per dark mass unit is identical within the errors, ≈1.0(±0.3) × 10<SUP>-9</SUP>. The total stellar mass derived for NGC 4486 is 6.8(±1.1) × 10<SUP>11</SUP> M⊙ with a baryonic mass fraction f<SUB>b</SUB>= 0.08(±0.01). Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
description |
As shown in previous works, globular clusters (GCs) can be used to trace the overall structure of the diffuse stellar populations in early-type galaxies if the number of clusters per unit stellar mass depends on metallicity. In this paper we further test this assumption in the galaxy NGC 4486 (M87) by combining several data sources. The results show that GCs allow the mapping of the galaxy in terms of the surface brightness profile, integrated colour gradient, chemical abundance and mass-to-luminosity ratios up to 1000arcsec (or 80.4kpc) from its centre (i.e. some 10 effective radii). The analysis indicates the presence of a dominant high-metallicity bulge associated with the red globulars, whose ellipticity increases outwards, and of a more flattened low-metallicity halo connected with the blue globulars. The chemical abundance gradient of the composite stellar population is remarkably similar to that inferred from X-ray observations of hot gas. The mass-metallicity spectrum of the stellar population can, in principle, be understood in terms of inhomogeneous enrichment models. In turn, the distribution of the bluest GCs, and lowest metallicity halo stars, has an intriguing similarity with that of dark matter, a feature shared with NGC 1399. Also, in these two galaxies, the number of blue GCs per dark mass unit is identical within the errors, ≈1.0(±0.3) × 10<SUP>-9</SUP>. The total stellar mass derived for NGC 4486 is 6.8(±1.1) × 10<SUP>11</SUP> M⊙ with a baryonic mass fraction f<SUB>b</SUB>= 0.08(±0.01). |
publishDate |
2012 |
dc.date.none.fl_str_mv |
2012 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo 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://sedici.unlp.edu.ar/handle/10915/84681 |
url |
http://sedici.unlp.edu.ar/handle/10915/84681 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.20341.x |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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openAccess |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
dc.format.none.fl_str_mv |
application/pdf 635-650 |
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