Statistics Of Giant Radio Halos: Expectations, and Recent (GMRT) and Future (LOFAR, LWA) Observations

Details Statistics Of Giant Radio Halos: Expectations, and Recent (GMRT) and Future (LOFAR, LWA) Observations Statistics Of Giant Radio Halos: Expectations, and Recent (GMRT) and Future (LOFAR, LWA) Observations

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..12e..46c&link_type=abstract

Long Wavelength Astrophysics, 26th meeting of the IAU, Joint Discussion 12, 21 August 2006, Prague, Czech Republic, JD12, #46

Astronomy and Astrophysics

Astrophysics

Scientific paper

A promising possibility to expalain the existence of giant radio halos (GRHs) in galaxy clusters is given by the "in situ" particle re-acceleration model. This model seems to reproduce the observational properties of the diffuse radio emission. On the other hand the cosmological evolution of GRHs, their statistical properties, and their physical connection with cluster mergers are still issues to be investigated. We have recently carried out the first calculations aimed at deriving the main statistical properties of GRHs in the framework of the electron re-acceleration scenario (Cassano & Brunetti 2005; Cassano, Brunetti, Setti 2006). These calculations allow to derive the occurrence of GRHs with the mass of the parent clusters, the evolution of this occurrence with redshift, and the Luminosity Functions and Number Counts of GRHs at different observing frequencies. The expected occurrence and Number Counts can be tested with present (GMRT and VLA) and future (LOFAR, LWA and SKA) observations. In particular to derive the occurrence of GRHs in the redshift bin 0.2-0.4 and to test our expectations we have carried out relatively deep observations of about 50 massive galaxy clusters at 600 MHz with the GMRT in India. Occurrence with cluster mass: In the first part of this talk I will present the status of the GMRT project (Venturi et al. 2006, submitted), and a first comparison between our theoretical expectations on the occurrence of GRHs with cluster mass and the GMRT results (including also comparison with observations in the redshift bin 0.05-0.2; Giovannini et al. 1999). Number Counts of GRHs: In the second part of the talk I will focus on our results obtained for the Luminosity Functions and for the Number Counts of GRHs at different observing frequencies (50 MHz -- 1.4 GHz). These expectations are important for the interpretation of the future observations with LOFAR and LWA.

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