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- 저자 : SETTI G. (검색결과 2 건)
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PROPERTIES AND SPECTRAL BEHAVIOUR OF CLUSTER RADIO HALOS
L. FERETTI,G. BRUNETTI,G. GIOVANNINI,N. KASSIM,E. ORRU,G. SETTI 한국천문학회 2004 Journal of The Korean Astronomical Society Vol.37 No.5
Several arguments have been presented in the literature to support the connection between radiohalos and cluster mergers. The spectral index distributions of the halos in A665 and A2163 provide anew strong conrmation of this connection, i.e. of the fact that the cluster merger plays an importantrole in the energy supply to the radio halos. Features of the spectral index (attening and patches)are indication of a complex shape of the radiating electron spectrum, and are therefore in support ofelectron reacceleration models. Regions of atter spectrum are found to be related to the recent merger.In the undisturbed cluster regions, instead, the spectrum steepens with the distance from the clustercenter. The plot of the integrated spectral index of a sample of halos versus the cluster temperatureindicates that clusters at higher temperature tend to host halos with atter spectra. This correlationprovides further evidence of the connection between radio emission and cluster mergers.
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OCCURENCE AND LUMINOSITY FUNCTIONS OF GIANT RADIO HALOS FROM MAGNETO-TURBULENT MODEL
CASSANO R.,BRUNETTI G.,SETTI G. The Korean Astronomical Society 2004 Journal of The Korean Astronomical Society Vol.37 No.5
We calculate the probability to form giant radio halos (${\~}$ 1 Mpc size) as a function of the mass of the host clusters by using a Statistical Magneto-Turbulent Model (Cassano & Brunetti, these proceedings). We show that the expectations of this model are in good agreement with the observations for viable values of the parameters. In particular, the abrupt increase of the probability to find radio halos in the more massive galaxy clusters ($M {\ge} 2{\times}10^{15} M_{\bigodot}$) can be well reproduced. We calculate the evolution with redshift of such a probability and find that giant radio halos can be powered by particle acceleration due to MHD turbulence up to z${\~}$0.5 in a ACDM cosmology. Finally, we calculate the expected Luminosity Functions of radio halos (RHLFs). At variance with previous studies, the shape of our RHLFs is characterized by the presence of a cut-off at low synchrotron powers which reflects the inefficiency of particle acceleration in the case of less massive galaxy clusters.
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