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Studying the Cosmological Evolution of Supermassive Black Holes with LOFAR

This research aims to investigate the cosmological evolution of supermassive black holes using LOFAR, focusing on topics such as accretion over cosmological timescales, active galactic nuclei, and galaxy evolution. By studying the nuclear properties of AGN, a link between jet power and accretion power can be established. The LOFAR's excellent sensitivity will expand our knowledge of the faint end of radio luminosity function and provide insights into the feedback from radio-emitting AGN.

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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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