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A synthetic view of AGN evolution and Supermassive black holes growth

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.

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A synthetic view of AGN evolution and Supermassive black holes growth

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  1. 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

  2. Outline • 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

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

  4. 0 -5 1 -4 2 -3 3 -2 4 -1 0 5 6 1 2 7 8 3 9 4 Log R/RS Log R/pc A logarithmic view of the AGN-galaxy connection [VLA/LOFAR] Radio Lobe Binding Energies Eb,≈4  1048 ergs Eb,BH,8≈1061 ergs Eb,gal,11≈1059 ergs Eb,Coma≈1064 ergs Bulge TOR [IR] RB Jet [VLBI/-rays] BLR [Opt/UV spec.] Rvir,12 AD [X-rays] Rsub disc Risco

  5. Q: How does the feedback loop close? OrIs 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. GX 339-4 Fender et al. 1999 Hot vs. cold? Low vs. high mdot? XRB examples

  7. XRB: low/hard state as jet-dominated RIAF • 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 Falcke and Biermann ’96; Heinz and Sunyaev 2003; Merloni et al 2003

  8. The Fundamental Plane of active black holes

  9. The Fundamental Plane of active black holes Merloni, Heinz & Di Matteo (2003) Gültekin et al. (2009)

  10. AGN feedback: evidence on cluster scale • 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

  11. Core Radio/LKin relation Log Lkin=0.81 Log L5GHz +11.9 Slope=0.81 Observed LR (beaming) Derived from FP relation Monte Carlo simulation: Statistical estimates of mean Lorentz Factor ~8 Not a distance effect: partial correlation analysis Pnul=2 10-4 Merloni and Heinz (2007)

  12. Low Power AGN are jet dominated • The observed slope (0.49±0.06) is consistent with radiatively inefficient “jet dominated” models Radiative power dominates output Kinetic power dominates output Log Lkin/LEdd=0.49 Log Lbol/Ledd - 0.78 Log Log Merloni and Heinz (2007)

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

  14. LR LX0.6-0.7 M0.7-0.8 LKIN LR0.7-0.8 LKIN /LEDD LX/LEDD0.5 LKIN,JEt~ Lbol Basic scaling laws (working hypothesis) LLAGN (L/Ledd<0.01) Powerful Jets (L/Ledd>0.01)

  15. Accretion diagram for LMXB & AGN Model parameter New “Blazar Sequence” Ghisellini and Tavecchio (2009) LK (low-kinetic; LLAGN, FRI) HK (high-kinetic; RLQ, FRII) HR (high-radiative; RQQ) (Blandford & Begelman 1999, Körding et al. 2007, Merloni and Heinz 2008)

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

  17. Continuity equation for SMBH growth = 0 Need to know simultaneously mass function(M,t0) and accretion rate distribution F(dM/dt,M,t) [“Fueling function”] luminosity function mass function Cavaliere et al. (1973); Small & Blandford (1992); Marconi et al. (2004); Merloni (2004)

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

  19. Bivariate distributions NLAGN BLAGN Z=1.0

  20. Bivariate distributions NLAGN BLAGN Z=2.0

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

  22. Perez-Gonzalez et al. 2008 Anti-hierarchical growth of structures Gal. growth times [Gyr] BH growth times [Gyr] 1M$ Question: What (if any) is the physical link between these two apparently related evolutionary paths?

  23. The Kinetic Energy output of SMBH

  24. Accretion diagram for LMXB & AGN Model parameter LK (low-kinetic; LLAGN, FRI) HK (high-kinetic; RLQ, FRII) HR (high-radiative; RQQ) (Blandford & Begelman 1999, Körding et al. 2007, Merloni and Heinz 2008)

  25. SMBH growth: weighting modes Log Lkin= 45.2 x 0.81 Log (P1.4,core /1025) (Merloni & Heinz 2007) 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”) Heinz, Merloni and Schwaab (2007) Körding, Jester and Fender (2007) Cattaneo and Best (2009)

  26. SMBH growth: weighting modes Log Lkin= 45.2 x 0.81 Log (P1.4,core /1025) (Merloni & Heinz 2007) 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”) Heinz, Merloni and Schwaab (2007) Körding, Jester and Fender (2007) Cattaneo and Best (2009)

  27. Conclusions • 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).

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