1. 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 Merloni Excellence Cluster Universe, Garching, Max-Planck Institut für Extraterrestrische Physik With Sebastian Heinz (Univ. of Wisconsin)

2. 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

3. The standard view of the AGN-galaxy connection Image credit: Aurore Simonnet, Sonoma State University

4. Log R/R S 0123456789 Log R/pc -5-4-3-201234 R isco R sub RBRB 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 Energies E b,  ≈4  10 48 ergs E b,BH,8 ≈10 61 ergs E b,gal,11 ≈10 59 ergs E b,Coma ≈10 64 ergs R vir,12

5. 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?

6. Hot vs. cold? Low vs. high mdot? XRB examples GX 339-4 Fender et al. 1999

7. 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 L Kin ~ Accretion rate Independent of geometry and jet acceleration mechanisms, it can be shown that L R ~M 17/12 mdot 17/12 for flat radio spectra from compact, self-absorbed synchrotron The observed radio-X-ray correlation (L R ~L X 0.7 ) implies: X-ray emission is radiatively inefficient (L X ~Mdot 2 ) L Kin ~ L R 1.4 XRB: low/hard state as jet-dominated RIAF

8. The Fundamental Plane of active black holes

9. Merloni, Heinz & Di Matteo (2003) Gültekin et al. (2009)

10. 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

11. Merloni and Heinz (2007) Observed L R (beaming) Derived from FP relation Monte Carlo simulation: Statistical estimates of mean Lorentz Factor  ~8 Slope=0.81 Log L kin =0.81 Log L 5GHz +11.9 Not a distance effect: partial correlation analysis P nul =2  10 -4 Core Radio/L Kin relation

12. Low Power AGN are jet dominated Log Merloni and Heinz (2007) Log L kin /L Edd =0.49 Log L bol /L edd - 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

13. Powerful jets: Clues from FERMI Blazars Ghisellini et al. 2009

14. Basic scaling laws (working hypothesis) L R  L X 0.6-0.7 M 0.7-0.8 L KIN  L R 0.7-0.8 L KIN /L EDD  L X /L EDD 0.5 LLAGN (L/L edd <0.01) L KIN,JEt  ~ L bol Powerful Jets (L/L edd >0.01)

15. (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)

16. A synthetic view of SMBH growth: the “radiative” sector

17. = 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,t 0 ) and accretion rate distribution F(dM/dt,M,t) [“Fueling function”] mass functionluminosity function

18. Bivariate distributions Z=0.3 Mass function of Emission Line AGN NLAGN BLAGN Greene and Ho 2007

19. Bivariate distributions Z=1.0 NLAGN BLAGN

20. Bivariate distributions Z=2.0 NLAGN BLAGN

21. Mass & Fueling functions evolution Log M=7 Log M=9 z=0.1 z=4

22. 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 growth times [Gyr] Gal. growth times [Gyr]

23. The Kinetic Energy output of SMBH

24. (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)

25. SMBH growth: weighting modes Heinz, Merloni and Schwaab (2007) Körding, Jester and Fender (2007) Cattaneo and Best (2009) Log L kin = 44.1 x 0.4 Log (P 1.4 /10 25 ) (Birzan et al. 2004, “cavity power”) Log L kin = 44.2 x 0.8 Log (P 1.4 /10 25 ) (Willott et al. 1999, “synchrotron power”) Log L kin = 45.2 x 0.81 Log (P 1.4,core /10 25 ) (Merloni & Heinz 2007)

26. SMBH growth: weighting modes Heinz, Merloni and Schwaab (2007) Körding, Jester and Fender (2007) Cattaneo and Best (2009) Log L kin = 44.1 x 0.4 Log (P 1.4 /10 25 ) (Birzan et al. 2004, “cavity power”) Log L kin = 44.2 x 0.8 Log (P 1.4 /10 25 ) (Willott et al. 1999, “synchrotron power”) Log L kin = 45.2 x 0.81 Log (P 1.4,core /10 25 ) (Merloni & Heinz 2007)

27. AGN obey simple scaling laws, at least for low accretion rates Main parameters are M and L/L Edd 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 L kin ~ L core,5GHz 0.7-0.8 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