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Studying the Cosmological evolution of supermassive black holes with LOFAR

Studying the Cosmological evolution of supermassive black holes with LOFAR. Andrea Merloni Excellence Cluster Universe & Max-Planck Institut für Extraterrestrische Physik Garching, Germany. Picture from Di Matteo et al. (2007). “Astrophysics with E-LOFAR”, Hamburg, 18/9/2008.

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Studying the Cosmological evolution of supermassive black holes with LOFAR

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  1. Studying the Cosmological evolution of supermassive black holes with LOFAR Andrea Merloni Excellence Cluster Universe & Max-Planck Institut für Extraterrestrische Physik Garching, Germany Picture from Di Matteo et al. (2007) “Astrophysics with E-LOFAR”, Hamburg, 18/9/2008

  2. Ω*BH≈710-5[Fukugita & Peebles (2007)] ΩSMBH≈2.710-6 Accretion over cosmological times, Active Galactic Nuclei, galaxy evolution Stellar physics, SN explosions, GRB M87 Sgr A* Black Holes in the local Universe Ωbaryon≈4.510-2 ;Ωstars≈2.510-3

  3. Best constraints on high-z (z>3) X-ray selected AGN evolution (XMM-COSMOS) Brusa et al. 2008 Accretion power: hard X-rays census Hopkins and Beacom (2006) Absorption-corrected X-ray LF, a, + contribution of Compton thick AGN from XRB synthesis model (~20-30%) of total grown mass

  4. Perez-Gonzalez et al.(2007) SMBH vs TOTAL stellar mass densities rad=0.07 3 1 z

  5. Radio cores scaling with M and mdot A “fundamental plane” of active BHs [Merloni et al. 2003; Falcke et al. 2004] See also Ho 2002; Greene, Ho and Ulvestad 2003 R*=(FR/Fbol)(max/5GHz) Log Log Log Log

  6. Using the FP to search for mode changes LLAGN, FRI RLQ,FRII RQQ

  7. Low Power AGN are jet dominated • By studying the nuclear properties of the AGN we can establish a link between jet power and accretion power • The observed slope (0.50±0.045) is perfectly consistent with radiatively inefficient “jet dominated” models (see E. Churazov’s talk) Cyg X-1 Log Lkin/LEdd=0.49 Log Lbol/Ledd - 0.78 Merloni and Heinz (2007)

  8. Extended Radio/LKin relation Lobes only Total - Larger scatter: aging, entrainment, intrinsic differences in B field strength and particle content. - Use cut-off freq. to account for aging gives tighter relation Bîrzan et al. (2008)

  9. Core Radio/LKin relation: effects of beaming Log Lkin=0.81 Log L5GHz +11.9 Slope=0.81 Slope=0.54 Observed LR (beaming) Derived from FP relation Monte Carlo simulation: Statistical estimates of mean Lorentz Factor~8 Merloni and Heinz (2007)

  10. Kinetic Energy output and efficiency Koerding, Jester and Fender (2007) Merloni and Heinz. (2008)

  11. Issues for (E-)LOFAR… • First and foremost, LOFAR excellent sensitivity will crucially expand our knowledge of the faint end of RLF (and extend it to high z) • Feedback from radio-emitting AGN important, but: • How to routinely calculate kinetic power output? • Multi-wavelength approach: Low- and High-freq radio obs + X-rays • Two steps are needed • Deep pointings of nearby radio galaxies, jets and clusters to calibrate Lradio vs. Lkin relation • Use LOFAR surveys to build robust kinetic luminosity function • Arcsec resolution crucial for faint AGN identification!

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