A First Estimate of Radio Halo Statistics from Large-Scale Cosmological Simulation
Abstract
In this paper, we present a first estimate based on a cosmological gas dynamics simulation of galaxy cluster radio halo counts to be expected in forthcoming low-frequency radio surveys. Our estimate is based on a FLASH simulation of the ΛCDM model for which we have assigned radio power to clusters via a model that relates radio emissivity to cluster magnetic field strength, intracluster turbulence, and density. We vary several free parameters of this model and find that radio halo number counts vary by up to a factor of two for average magnetic fields ranging from 0.2 to 3.1 μG. However, we predict significantly fewer low-frequency radio halos than expected from previous semi-analytic estimates, although this discrepancy could be explained by frequency-dependent radio halo probabilities as predicted in reacceleration models. We find that upcoming surveys will have difficulty in distinguishing models because of large uncertainties and low number counts. Additionally, according to our modeling we find that expected number counts can be degenerate with both reacceleration and hadronic secondary models of cosmic-ray generation. We find that relations between radio power and mass and X-ray luminosity may be used to distinguish models, and by building mock radio sky maps we demonstrate thatmore »
- Authors:
-
- Univ. of Illinois at Urbana-Champaign, Urbana, IL (United States). Dept. of Physics; Inst. d'Astrophysique de Paris, Paris (France). UPMC, and CNRS; Ohio State Univ., Columbus, OH (United States). Center for Cosmology and Astro-Particle Physics
- Univ. of Illinois at Urbana-Champaign, Urbana, IL (United States). Dept. of Astronomy, and National Center for Supercomputing Applications
- Publication Date:
- Research Org.:
- Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1565014
- Grant/Contract Number:
- AC05-00OR22725; FG02-97ER25308
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 759; Journal Issue: 2; Journal ID: ISSN 0004-637X
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; galaxies; clusters; intracluster medium; hydrodynamics; magnetic fields
Citation Formats
Sutter, P. M., and Ricker, P. M. A First Estimate of Radio Halo Statistics from Large-Scale Cosmological Simulation. United States: N. p., 2012.
Web. doi:10.1088/0004-637x/759/2/92.
Sutter, P. M., & Ricker, P. M. A First Estimate of Radio Halo Statistics from Large-Scale Cosmological Simulation. United States. https://doi.org/10.1088/0004-637x/759/2/92
Sutter, P. M., and Ricker, P. M. Wed .
"A First Estimate of Radio Halo Statistics from Large-Scale Cosmological Simulation". United States. https://doi.org/10.1088/0004-637x/759/2/92. https://www.osti.gov/servlets/purl/1565014.
@article{osti_1565014,
title = {A First Estimate of Radio Halo Statistics from Large-Scale Cosmological Simulation},
author = {Sutter, P. M. and Ricker, P. M.},
abstractNote = {In this paper, we present a first estimate based on a cosmological gas dynamics simulation of galaxy cluster radio halo counts to be expected in forthcoming low-frequency radio surveys. Our estimate is based on a FLASH simulation of the ΛCDM model for which we have assigned radio power to clusters via a model that relates radio emissivity to cluster magnetic field strength, intracluster turbulence, and density. We vary several free parameters of this model and find that radio halo number counts vary by up to a factor of two for average magnetic fields ranging from 0.2 to 3.1 μG. However, we predict significantly fewer low-frequency radio halos than expected from previous semi-analytic estimates, although this discrepancy could be explained by frequency-dependent radio halo probabilities as predicted in reacceleration models. We find that upcoming surveys will have difficulty in distinguishing models because of large uncertainties and low number counts. Additionally, according to our modeling we find that expected number counts can be degenerate with both reacceleration and hadronic secondary models of cosmic-ray generation. We find that relations between radio power and mass and X-ray luminosity may be used to distinguish models, and by building mock radio sky maps we demonstrate that surveys such as LOFAR may have sufficient resolution and sensitivity to break this model degeneracy by imaging many individual clusters.},
doi = {10.1088/0004-637x/759/2/92},
journal = {The Astrophysical Journal},
number = 2,
volume = 759,
place = {United States},
year = {Wed Oct 10 00:00:00 EDT 2012},
month = {Wed Oct 10 00:00:00 EDT 2012}
}
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