a synthetic view of agn evolution and supermassive black holes growth
DESCRIPTION
Andrea Merloni Excellence Cluster Universe, Garching, Max-Planck Institut für Extraterrestrische Physik With Sebastian Heinz (Univ. of Wisconsin). 5GHz, VLA image of Cyg A by R. Perley. A synthetic view of AGN evolution and Supermassive black holes growth. Leiden 25/11/2009. Outline. - PowerPoint PPT PresentationTRANSCRIPT
A synthetic view of AGN evolution and Supermassive black holes growth
Leiden 25/11/2009
5GHz, VLA image of Cyg A by R. Perley
Andrea MerloniExcellence Cluster Universe, Garching,
Max-Planck Institut für Extraterrestrische Physik
With Sebastian Heinz (Univ. of Wisconsin)
• Accretion modes
• XRB analogy and scaling laws
• Cosmological evolution (z<3-4)
• Continuity equation, mass and redshift dependence of the fuelling rate
• Kinetic vs. radiative feedback
Outline
The standard view of the AGN-galaxy connection
•Image credit: Aurore Simonnet, Sonoma State University
Log R/RS 0 1 2 3 4 5 6 7 8 9
Log R/pc -5 -4 -3 -2 -1 0 1 2 3 4
Risco
Rsub
RB
Bulge
disc
Radio Lobe
Jet[VLBI/-rays]
TOR [IR]
BLR[Opt/UV spec.]
AD [X-rays]
A logarithmic view of the AGN-galaxy connection
[VLA/LOFAR]
Binding EnergiesEb,≈4 1048 ergs
Eb,BH,8≈1061 ergs
Eb,gal,11≈1059 ergs
Eb,Coma≈1064 ergs
Rvir,12
Q: How does the feedback loop close? Or
Is the accretion (and energy release) mode of an AGN dictated by the internal energy of the
accreting gas, or simply by its overall rate?
Hot vs. cold? Low vs. high mdot? XRB examples
GX 339-4Fender et al. 1999
Falcke and Biermann ’96; Heinz and Sunyaev 2003; Merloni et al 2003
•Strong correlation between radio and X-ray emission in low/hard state (Gallo+ 2003)
•Assume jet power LKin~ Accretion rate
•Independent of geometry and jet acceleration mechanisms, it can be shown that LR~M17/12mdot17/12 for flat radio spectra from compact, self-absorbed synchrotron
•The observed radio-X-ray correlation (LR~LX0.7) implies:
• X-ray emission is radiatively inefficient (LX~Mdot2)
• LKin ~ LR1.4
XRB: low/hard state as jet-dominated RIAF
The Fundamental Plane of active black holes
The Fundamental Plane of active black holes
Merloni, Heinz & Di Matteo (2003)Gültekin et al. (2009)
• 1 Msec observation of the core of the Perseus Cluster with Chandra; True color image made from 0.3-1.2 (red), 1.2-2 (green), 2-7 (blue) keV photons
• First direct evidence of ripples, sound waves and shocks in the hot ICM
• Radio maps reveal close spatial coincidence between X-ray morphology and AGN-driven radio jets
(Birzan et al. 2004, 2008; Allen et al. 2006; Rafferty et al. 2006, etc.)
Fabian et al. 2006
AGN feedback: evidence on cluster scale
Merloni and Heinz (2007)
Observed LR (beaming)Derived from FP relation
Monte Carlo simulation:Statistical estimates ofmean Lorentz Factor ~8
Slope=0.81Log Lkin=0.81 Log L5GHz +11.9
Not a distance effect: partial correlation analysis Pnul=2 10-4
Core Radio/LKin relation
Low Power AGN are jet dominated
Log
Log
Merloni and Heinz (2007)
Log Lkin/LEdd=0.49 Log Lbol/Ledd - 0.78
• The observed slope (0.49±0.06) is consistent with radiatively inefficient “jet dominated” models
Kinetic power dominates output
Radiative power dominates output
Powerful jets: Clues from FERMI Blazars
Ghisellini et al. 2009
Basic scaling laws (working hypothesis)
LR LX0.6-0.7 M0.7-0.8
LKIN LR0.7-0.8
LKIN /LEDD LX/LEDD0.5
LLAGN (L/Ledd<0.01)
LKIN,JEt~ Lbol
Powerful Jets (L/Ledd>0.01)
(Blandford & Begelman 1999, Körding et al. 2007, Merloni and Heinz 2008)
Accretion diagram for LMXB & AGN
Model parameter
LK (low-kinetic; LLAGN, FRI)
HK (high-kinetic; RLQ, FRII)
HR (high-radiative; RQQ)
New “Blazar Sequence”Ghisellini and Tavecchio (2009)
A synthetic view of SMBH growth:the “radiative” sector
= 0
Cavaliere et al. (1973); Small & Blandford (1992); Marconi et al. (2004); Merloni (2004)
Continuity equation for SMBH growth
Need to know simultaneously mass function (M,t0) and accretion rate distribution F(dM/dt,M,t) [“Fueling function”]
mass functionluminosity function
Bivariate distributions
Z=0.3
Mass function of Emission Line AGN
NLAGNBLAGN
Greene and Ho 2007
Bivariate distributions
Z=1.0
NLAGNBLAGN
Bivariate distributions
Z=2.0
NLAGNBLAGN
Mass & Fueling functions evolution
Log M=7
Log M=9
z=0.1
z=4
Perez-Gonzalez et al. 2008
Anti-hierarchical growth of structures
1M$ Question:
What (if any) is the physical link between these two apparently related evolutionary paths?
BH
gro
wth
tim
es
[Gyr]
Gal. g
row
th t
imes
[Gyr]
The Kinetic Energy output of SMBH
(Blandford & Begelman 1999, Körding et al. 2007, Merloni and Heinz 2008)
Accretion diagram for LMXB & AGN
Model parameter
LK (low-kinetic; LLAGN, FRI)
HK (high-kinetic; RLQ, FRII)
HR (high-radiative; RQQ)
SMBH growth: weighting modes
Heinz, Merloni and Schwaab (2007)
Körding, Jester and Fender (2007)
Cattaneo and Best (2009)
Log Lkin= 44.1 x 0.4 Log (P1.4 /1025)(Birzan et al. 2004, “cavity power”)
Log Lkin= 44.2 x 0.8 Log (P1.4 /1025)(Willott et al. 1999, “synchrotron power”)
Log Lkin= 45.2 x 0.81 Log (P1.4,core /1025)(Merloni & Heinz 2007)
SMBH growth: weighting modes
Heinz, Merloni and Schwaab (2007)
Körding, Jester and Fender (2007)
Cattaneo and Best (2009)
Log Lkin= 44.1 x 0.4 Log (P1.4 /1025)(Birzan et al. 2004, “cavity power”)
Log Lkin= 44.2 x 0.8 Log (P1.4 /1025)(Willott et al. 1999, “synchrotron power”)
Log Lkin= 45.2 x 0.81 Log (P1.4,core /1025)(Merloni & Heinz 2007)
• AGN obey simple scaling laws, at least for low accretion rates
• Main parameters are M and L/LEdd
• SMBH grow with a broad accretion rate distribution (be very careful when discussing AGN fractions, AGN lifetimes, etc.)
• The anti-hierarchical trend is clearly seen in the low-z evolution of SMBH mass function.
• Physically motivated scaling Lkin ~ Lcore,5GHz0.7-0.8
• Feedback from “Low-luminosity AGN” is most likely dominated by kinetic energy
• The efficiency with which growing black holes convert mass into mechanical energy is 0.3-0.5% (but strongly dependent on BH mass and redshift).
Conclusions