Ram pressure profiles in galaxy groups and clusters

Using a hybrid method that combines non-radiative hydrodynamical simulations with a semianalytic model of galaxy formation, we determine the ram pressure experienced by galaxies in haloes with virial masses 12.5 ≤ log (M<sub>200</sub>/ h<sup>−1</sup> M⊙) < 15.35 as a funct...

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Detalles Bibliográficos
Autores principales: Tecce, Tomás Enrique, Cora, Sofía Alejandra, Tissera, Patricia Beatriz
Formato: Articulo
Lenguaje:Inglés
Publicado: 2011
Materias:
Astronomía
methods: numerical
galaxies: clusters: general
galaxies: clusters: intracluster medium
galaxies: evolution
galaxies: groups: general
intergalactic medium
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/93549
http://mnras.oxfordjournals.org/content/416/4/3170
https://ri.conicet.gov.ar/handle/11336/9960
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-93549
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
methods: numerical
galaxies: clusters: general
galaxies: clusters: intracluster medium
galaxies: evolution
galaxies: groups: general
intergalactic medium
spellingShingle Astronomía
methods: numerical
galaxies: clusters: general
galaxies: clusters: intracluster medium
galaxies: evolution
galaxies: groups: general
intergalactic medium
Tecce, Tomás Enrique
Cora, Sofía Alejandra
Tissera, Patricia Beatriz
Ram pressure profiles in galaxy groups and clusters
topic_facet Astronomía
methods: numerical
galaxies: clusters: general
galaxies: clusters: intracluster medium
galaxies: evolution
galaxies: groups: general
intergalactic medium
description Using a hybrid method that combines non-radiative hydrodynamical simulations with a semianalytic model of galaxy formation, we determine the ram pressure experienced by galaxies in haloes with virial masses 12.5 ≤ log (M<sub>200</sub>/ h<sup>−1</sup> M⊙) < 15.35 as a function of the halocentric distance, for redshifts 0 ≤ z ≤ 3. The ram pressure is calculated with a self-consistent method that uses the simulation gas particles to obtain the properties of the intergalactic medium. The ram pressure profiles obtained can be well described by beta profile models, with parameters that depend on redshift and halo virial mass in a simple fashion. The fitting formulae provided here will prove useful to include ram pressure effects into semi-analytic models based on methods that lack gas physics, such as dark-matter-only simulations or the Press–Schechter formalism.
format Articulo
Articulo
author Tecce, Tomás Enrique
Cora, Sofía Alejandra
Tissera, Patricia Beatriz
author_facet Tecce, Tomás Enrique
Cora, Sofía Alejandra
Tissera, Patricia Beatriz
author_sort Tecce, Tomás Enrique
title Ram pressure profiles in galaxy groups and clusters
title_short Ram pressure profiles in galaxy groups and clusters
title_full Ram pressure profiles in galaxy groups and clusters
title_fullStr Ram pressure profiles in galaxy groups and clusters
title_full_unstemmed Ram pressure profiles in galaxy groups and clusters
title_sort ram pressure profiles in galaxy groups and clusters
publishDate 2011
url http://sedici.unlp.edu.ar/handle/10915/93549
http://mnras.oxfordjournals.org/content/416/4/3170
https://ri.conicet.gov.ar/handle/11336/9960
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AT corasofiaalejandra rampressureprofilesingalaxygroupsandclusters
AT tisserapatriciabeatriz rampressureprofilesingalaxygroupsandclusters
bdutipo_str Repositorios
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