Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias

We have performed a series of N-body experiments including the effects of a massive domiannt background that follows Schuster's density law in order to simulate clusters of galaxies in which a smoothly distributed dark component is present. The existence of this backgroud is inferred from the w...

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Detalles Bibliográficos
Autores principales: Navarro, J., García-Lambas, D.
Formato: Articulo Comunicacion
Lenguaje:Español
Publicado: 1987
Materias:
Astronomía
Galaxias
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/132203
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-132203
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Español
topic Astronomía
Galaxias
spellingShingle Astronomía
Galaxias
Navarro, J.
García-Lambas, D.
Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
topic_facet Astronomía
Galaxias
description We have performed a series of N-body experiments including the effects of a massive domiannt background that follows Schuster's density law in order to simulate clusters of galaxies in which a smoothly distributed dark component is present. The existence of this backgroud is inferred from the weak luminosity segregation observed in clusters which, however, show several characteristics of well relaxes systems. The comparison of the velocity dispersion profiles of three clusters of galaxies (Coma, Perseus, and Virgo) with those obtaineed in the numerical experiments allows us to place some constraints on both the distribution and amount of distributed dark material in these clusters. The profiles are rather insensitive to variations in the ratio of the background mass to the mass attached to galaxies (Mb/Mg), but exhibit a strong dependence on their relative concentration. We conclude that highly concentrated background models are not consistent with observations. We find a maximum value for the ratio of the gravitational radius of the galaxies and the background (Rg/Rb) (approximately 0.6) and using previous results (Navarro et al. 1986 Ap. and Sp. Sci. 123, 117) we conclude that virial theorem masses underestimate the total (Mb+Mg) of the clusters. As a final result, we derive a minimum value for the Mb/Mg ratio. All these conclusions could apply in general if Coma, Perseus and Virgo constitute a fair sample of the rich clusters of galaxies in the Universe.
format Articulo
Comunicacion
author Navarro, J.
García-Lambas, D.
author_facet Navarro, J.
García-Lambas, D.
author_sort Navarro, J.
title Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
title_short Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
title_full Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
title_fullStr Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
title_full_unstemmed Influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
title_sort influencia de la materia oscura en los perfiles de velocidad radial de cúmulos de galaxias
publishDate 1987
url http://sedici.unlp.edu.ar/handle/10915/132203
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bdutipo_str Repositorios
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