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Luigina Feretti Istituto di Radioastronomia INAF Bologna, Italy

Radio emission in clusters and connection to X-ray emission. Luigina Feretti Istituto di Radioastronomia INAF Bologna, Italy. SIMBOL-X: THE HARD X-RAY UNIVERSE IN FOCUS. Bologna 16 May 2007. OUTLINE. Diffuse cluster radio emission:  non-thermal components of the ICM

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Luigina Feretti Istituto di Radioastronomia INAF Bologna, Italy

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  1. Radio emission in clusters and connection to X-ray emission Luigina Feretti Istituto di Radioastronomia INAF Bologna, Italy SIMBOL-X: THE HARD X-RAY UNIVERSE IN FOCUS Bologna 16 May 2007

  2. OUTLINE • Diffuse cluster radio emission:  non-thermal components of the ICM • Link between radio emission and thermal X ray emission • Magnetic field determination from Rotation Measure • Non-thermal hard X-ray emission

  3. Feretti et al. 2001 A2163

  4. Diffuse Radio Sources in clusters : 1 - radio halos : similar distribution as X-ray gas  Mpc size

  5. Halos A665 A2319 A2255

  6. Link between radio and X-ray emission Cassano Brunetti Setti 2006 A2163 – Feretti et al. 2001 A2744 – Orru’ et al. 2007 Particle reacceleration from turbulence in merging clusters

  7. Rottgering et al. A3667

  8. Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics : elongated, at cluster peripheries  Mpc

  9. A2255 A548b z= 0.0809 Relic size 730 kpc Feretti et al. 2003 Feretti et al. 1997

  10. Giovannini & Feretti 2004 Particle reacceleration from Shock waves in merging clusters

  11. Transfer of energy from merger to halos and relics shocks turbulence (Ricker & Sarazin 2001) Color = temperature, Contours = X-ray brightness

  12. Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters Perseus Radio, Size = 350 kpc (Sijbring & De Bruyn 1993 )

  13. A2626 – Gitti et al. 2004 A2390 – Bacchi et al. 2003 P - 1.4 GHz Pcf

  14. Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters 4 – radio galaxies related to cD galaxies in cool core clusters, radio bubbles, ghost bubbles Perseus – Fabian et al 2000 Chandra (Böhringer et al ROSAT)  Confinement RBS797 – Gitti Feretti Schindler 2006

  15. Radio : Owen et al. X-ray : Böhringer et al ROSAT

  16. Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters 4 – radio galaxies related to cD galaxies in cool core clusters, radio bubbles, ghost bubbles 5 - central relics (intermediate between 2 and 4)

  17. Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters 4 – radio galaxies related to cD galaxies in cool core clusters, radio bubbles, ghost bubbles 5 - central relics (intermediate between 2 and 4)  all steep spectrum sources M E R G E R R E L A X E D

  18. Synchrotron radio emission : Magnetic fields :  G Mpc scales Relativistic particles :  GeV,  >> 1000 Mpc scales

  19.  RM Faraday Rotation • rotation of the plane of polarization of linearly polarized emission as it passes through a magneto-ionic plasma • -- due to the different phase velocities of the orthogonal circular modes • infer B if ne is known  X-ray 0  Kronberg 2002

  20. NON-THERMAL X-RAY EMISSION Relativistic electronsof   104  synchrotron emission in radio  inverse Compton emission in hard X ray Comparison between Radio and X-ray emissions gives estimates of magnetic field and relativistic particle energy density

  21. Evidence of relativistic particles from Inverse Compton emission in the Hard X-ray Detection in: - Coma (BeppoSAX: Fusco-Femiano et al. 2004, 2007) (RXTE: Rephaeli & Gruber 2002) - A 2256 (BeppoSAX: Fusco-Femiano 2005) - A 2319 (RXTE: Gruber & Rephaeli 2002) - A1750, IC1262 (Henriksen & Hudson 2004) possibly in A 85 (ROSAT: Bagchi et al. 1998, soft band ) Marginal detection in A 2199 (Kaastra et al. 1999 Upper limits in A119, A754 (Fusco-Femiano et al. 2002) A2163 (Feretti et al. 2001), Coma periphery: relic 1253+277  upper limit (Feretti & Neumann2006)

  22. Coma Thermal: T = 8.2 keV Non Thermal flux = 1.5 10-11 erg cm2 s1 in the 20–80 keV range B = 0.16 G Fusco-Femiano et al. 2004, 2007 need IMAGE of the HARD X-ray distribution

  23. FUTURE PROSPECTS • Comparison of radio and X-ray emission  structures spectra correlations interaction confinement • Accurate determination of thermal gas density to derive B field from the Rotation Measure • IC non-thermal emission  detection and images determination of B field value and e- energy

  24. THANK YOU

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