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Title: COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS

Abstract

Radio observations of galaxy clusters show that there are {mu}G magnetic fields permeating the intracluster medium (ICM), but it is hard to accurately constrain the strength and structure of the magnetic fields without the help of advanced computer simulations. We present qualitative comparisons of synthetic Very Large Array observations of simulated galaxy clusters to radio observations of Faraday rotation measure (RM) and radio halos. The cluster formation is modeled using adaptive mesh refinement magnetohydrodynamic simulations with the assumption that the initial magnetic fields are injected into the ICM by active galactic nuclei (AGNs) at high redshift. In addition to simulated clusters in Xu et al., we present a new simulation with magnetic field injections from multiple AGNs. We find that the cluster with multiple injection sources is magnetized to a similar level as in previous simulations with a single AGN. The RM profiles from simulated clusters, both |RM| and the dispersion of RM ({sigma}{sub RM}), are consistent at a first order with the radial distribution from observations. The correlations between the {sigma}{sub RM} and X-ray surface brightness from simulations are in a broad agreement with the observations, although there is an indication that the simulated clusters could be slightly overdensemore » and less magnetized with respect to those in the observed sample. In addition, the simulated radio halos agree with the observed correlations between the radio power versus the cluster X-ray luminosity and between the radio power versus the radio halo size. These studies show that the cluster-wide magnetic fields that originate from AGNs and are then amplified by the ICM turbulence match observations of magnetic fields in galaxy clusters.« less

Authors:
; ;  [1]; ;  [2];  [3];  [4]; ;  [5]
  1. Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)
  2. INAF-Osservatorio Astronomico di Cagliari, Poggio dei Pini, Strada 54, I-09012 Capoterra (Italy)
  3. Center for Astrophysics and Space Science, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093 (United States)
  4. Department of Astrophysical Science, Princeton University, Princeton, NJ 08544 (United States)
  5. INAF-Istituto di Radioastronomia, Via P.Gobetti 101, I-40129 Bologna (Italy)
Publication Date:
OSTI Identifier:
22086483
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 759; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTRONOMY; BRIGHTNESS; COMPARATIVE EVALUATIONS; COMPUTERIZED SIMULATION; CORRELATIONS; COSMOLOGY; FARADAY EFFECT; GALAXY CLUSTERS; GALAXY NUCLEI; LUMINOSITY; MAGNETIC FIELDS; RED SHIFT; SPATIAL DISTRIBUTION; TURBULENCE; UNIVERSE; X RADIATION

Citation Formats

Xu Hao, Li Hui, Collins, David C., Govoni, Federica, Murgia, Matteo, Norman, Michael L., Cen Renyue, Feretti, Luigina, and Giovannini, Gabriele, E-mail: hao_xu@lanl.gov, E-mail: hli@lanl.gov, E-mail: dccollins@lanl.gov, E-mail: mlnorman@ucsd.edu, E-mail: fgovoni@oa-cagliari.inaf.it, E-mail: matteo@oa-cagliari.inaf.it, E-mail: cen@astro.princeton.edu, E-mail: lferetti@ira.inaf.it, E-mail: ggiovann@ira.inaf.it. COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS. United States: N. p., 2012. Web. doi:10.1088/0004-637X/759/1/40.
Xu Hao, Li Hui, Collins, David C., Govoni, Federica, Murgia, Matteo, Norman, Michael L., Cen Renyue, Feretti, Luigina, & Giovannini, Gabriele, E-mail: hao_xu@lanl.gov, E-mail: hli@lanl.gov, E-mail: dccollins@lanl.gov, E-mail: mlnorman@ucsd.edu, E-mail: fgovoni@oa-cagliari.inaf.it, E-mail: matteo@oa-cagliari.inaf.it, E-mail: cen@astro.princeton.edu, E-mail: lferetti@ira.inaf.it, E-mail: ggiovann@ira.inaf.it. COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS. United States. doi:10.1088/0004-637X/759/1/40.
Xu Hao, Li Hui, Collins, David C., Govoni, Federica, Murgia, Matteo, Norman, Michael L., Cen Renyue, Feretti, Luigina, and Giovannini, Gabriele, E-mail: hao_xu@lanl.gov, E-mail: hli@lanl.gov, E-mail: dccollins@lanl.gov, E-mail: mlnorman@ucsd.edu, E-mail: fgovoni@oa-cagliari.inaf.it, E-mail: matteo@oa-cagliari.inaf.it, E-mail: cen@astro.princeton.edu, E-mail: lferetti@ira.inaf.it, E-mail: ggiovann@ira.inaf.it. Thu . "COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS". United States. doi:10.1088/0004-637X/759/1/40.
@article{osti_22086483,
title = {COMPARISONS OF COSMOLOGICAL MAGNETOHYDRODYNAMIC GALAXY CLUSTER SIMULATIONS TO RADIO OBSERVATIONS},
author = {Xu Hao and Li Hui and Collins, David C. and Govoni, Federica and Murgia, Matteo and Norman, Michael L. and Cen Renyue and Feretti, Luigina and Giovannini, Gabriele, E-mail: hao_xu@lanl.gov, E-mail: hli@lanl.gov, E-mail: dccollins@lanl.gov, E-mail: mlnorman@ucsd.edu, E-mail: fgovoni@oa-cagliari.inaf.it, E-mail: matteo@oa-cagliari.inaf.it, E-mail: cen@astro.princeton.edu, E-mail: lferetti@ira.inaf.it, E-mail: ggiovann@ira.inaf.it},
abstractNote = {Radio observations of galaxy clusters show that there are {mu}G magnetic fields permeating the intracluster medium (ICM), but it is hard to accurately constrain the strength and structure of the magnetic fields without the help of advanced computer simulations. We present qualitative comparisons of synthetic Very Large Array observations of simulated galaxy clusters to radio observations of Faraday rotation measure (RM) and radio halos. The cluster formation is modeled using adaptive mesh refinement magnetohydrodynamic simulations with the assumption that the initial magnetic fields are injected into the ICM by active galactic nuclei (AGNs) at high redshift. In addition to simulated clusters in Xu et al., we present a new simulation with magnetic field injections from multiple AGNs. We find that the cluster with multiple injection sources is magnetized to a similar level as in previous simulations with a single AGN. The RM profiles from simulated clusters, both |RM| and the dispersion of RM ({sigma}{sub RM}), are consistent at a first order with the radial distribution from observations. The correlations between the {sigma}{sub RM} and X-ray surface brightness from simulations are in a broad agreement with the observations, although there is an indication that the simulated clusters could be slightly overdense and less magnetized with respect to those in the observed sample. In addition, the simulated radio halos agree with the observed correlations between the radio power versus the cluster X-ray luminosity and between the radio power versus the radio halo size. These studies show that the cluster-wide magnetic fields that originate from AGNs and are then amplified by the ICM turbulence match observations of magnetic fields in galaxy clusters.},
doi = {10.1088/0004-637X/759/1/40},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 759,
place = {United States},
year = {2012},
month = {11}
}