REVISITING SCALING RELATIONS FOR GIANT RADIO HALOS IN GALAXY CLUSTERS

Many galaxy clusters host megaparsec-scale radio halos, generated by ultrarelativistic electrons in the magnetized intracluster medium. The X-ray luminosity and redshift-limited Extended GMRT Radio Halo Survey provides a rich and unique dataset for statistical studies of the halos. We uniformly anal...

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Bibliographic Details
Published in:The Astrophysical journal 2013-11, Vol.777 (2), p.1-14
Main Authors: Cassano, R, Ettori, S, Brunetti, G, Giacintucci, S, Pratt, G W, Venturi, T, Kale, R, Dolag, K, Markevitch, M
Format: Article
Language:English
Subjects:
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Clusters
Correlation
CORRELATIONS
COSMIC ELECTRONS
COSMIC RADIO SOURCES
Galactic clusters
Galactic halos
GALAXY CLUSTERS
GHZ RANGE
Halos
KEV RANGE
LUMINOSITY
Radio
RADIOASTRONOMY
RED SHIFT
RELATIVISTIC RANGE
Statistical methods
THERMODYNAMIC PROPERTIES
X RADIATION
X-RAY GALAXIES
X-rays
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Summary:Many galaxy clusters host megaparsec-scale radio halos, generated by ultrarelativistic electrons in the magnetized intracluster medium. The X-ray luminosity and redshift-limited Extended GMRT Radio Halo Survey provides a rich and unique dataset for statistical studies of the halos. We uniformly analyze the radio and X-ray data for the GMRT cluster sample, and use the new Planck Sunyaev-Zel'dovich (SZ) catalog to revisit the correlations between the power of radio halos and the thermal properties of galaxy clusters. Our bigger and more homogenous sample confirms that the X-ray luminous (L sub(500) > 5 x 10 super(44) erg s super(-1)) clusters branch into two populations-radio halos lie on the correlation, while clusters without radio halos have their radio upper limits well below that correlation. Bimodality of both correlations can be traced to clusters dynamics, with radio halos found exclusively in merging clusters. These results confirm the key role of mergers for the origin of giant radio halos, suggesting that they trigger the relativistic particle acceleration.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/777/2/141