Transcript 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.

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
Black Holes in the local Universe
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
Ωbaryon≈4.510-2 ; Ωstars≈2.510-3
Sgr A*
M87
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 (~2030%) of total grown mass
Best constraints on high-z
(z>3) X-ray selected AGN
evolution (XMM-COSMOS)
Brusa et al. 2008
SMBH vs TOTAL stellar mass densities
rad=0.07
3
1
z
Perez-Gonzalez et al.(2007)
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
R*=(FR/Fbol)(max/5GHz)
Log
Log
Using the
FP to search for mode changes
LLAGN, FRI
RLQ,FRII
RQQ
Low Power AGN are jet dominated
• By studying the nuclear
Cyg X-1
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
Merloni and Heinz (2007)
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
Bîrzan et al. (2008)
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)
Kinetic Energy output and efficiency
Merloni and Heinz. (2008)
Koerding, Jester and Fender (2007)
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!