Studying the Cosmological evolution of

supermassive black holes with

LOFAR

“Astrophysics with E-LOFAR”, Hamburg, 18/9/2008

Andrea MerloniExcellence Cluster Universe &

Max-Planck Institut für Extraterrestrische Physik

Garching, Germany Picture from Di Matteo et al. (2007)

Sgr A* M87

Black Holes in the local Universe

ΩSMBH≈2.710-6

Accretion over cosmological times, Active Galactic Nuclei, galaxy evolution

Ωbaryon≈4.510-2 ; Ωstars≈2.510-3

Ω*BH≈710-5 [Fukugita & Peebles (2007)]

Stellar physics, SN explosions, GRB

Accretion power: hard X-rays census

Hopkins and Beacom (2006)

Brusa et al. 2008

Best constraints on high-z (z>3) X-ray selected AGN evolution (XMM-COSMOS)

Absorption-corrected X-ray LF, a, + contribution of Compton thick AGN from XRB synthesis model (~20-30%) of total grown mass

SMBH vs TOTAL stellar mass densities

Perez-Gonzalez et al.(2007)z1 3

rad=0.07

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

Log Log

Log

Log

R*=(FR/Fbol)(max/5GHz)

Using the FP to search for mode changes

LLAGN, FRI RLQ,FRII

RQQ

Cyg X-1

Merloni and Heinz (2007)

• 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)

Log Lkin/LEdd=0.49 Log Lbol/Ledd - 0.78

Low Power AGN are jet dominated

Bîrzan et al. (2008)

Extended Radio/LKin relation

Total Lobes only

- Larger scatter: aging, entrainment, intrinsic differences in B field strength and particle content.- Use cut-off freq. to account for aging gives tighter relation

Merloni and Heinz (2007)

Observed LR (beaming)Derived from FP relation

Monte Carlo simulation:Statistical estimates ofmean Lorentz Factor~8

Slope=0.54

Slope=0.81Log Lkin=0.81 Log L5GHz +11.9

Core Radio/LKin relation: effects of beaming

Koerding, Jester and Fender (2007)

Kinetic Energy output and efficiency

Merloni and Heinz. (2008)

• 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!

Issues for (E-)LOFAR…