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Cosmological growth of SMBH: the kinetic luminosity function of AGN

5GHz, VLA image of Cyg A by R. Perley. Cosmological growth of SMBH: the kinetic luminosity function of AGN. Andrea Merloni Max-Planck Institute for Astrophysics & Sebastian Heinz MIT. IAU Symposium 238 – Prague 22/08/2006. Intro: Key questions.

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Cosmological growth of SMBH: the kinetic luminosity function of AGN

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  1. 5GHz, VLA image of Cyg A by R. Perley Cosmological growth of SMBH:the kinetic luminosity function of AGN Andrea Merloni Max-Planck Institute for Astrophysics & Sebastian Heinz MIT IAU Symposium 238 – Prague22/08/2006

  2. Intro: Key questions • Observed correlations (M-, Magorrian): How do they evolve athigh redshift? • Constraints on structure formation • Constraints on feedback models (“radio mode” vs. “quasar mode” in the cosmologists jargon) • What is the Kinetic Luminosity function of AGN, and how does it evolve? • Need to include knowledge of accretion physics

  3. Intro: Key questions • Observed correlations (M-, Magorrian): How do they evolve at high redshift? • Constraints on structure formation • Constraints on feedback models (“radio mode” vs. “quasar mode” in the cosmologists jargon) • What is the Kinetic Luminosity function of AGN, and how does it evolve? • Need to include knowledge of accretion physics

  4. Intro: Key questions • Observed correlations (M-, Magorrian): How do they evolve at high redshift? • Constraints on structure formation • Constraints on feedback models (“radio mode” vs. “quasar mode” in the cosmologists jargon) • What is the Kinetic Luminosity function of AGN, and how does it evolve? • Need to include knowledge of accretion physics

  5. Open questions in accretion theory • Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005)Þ jets/outflows dominate over radiation as power sinks. But is radiative efficiency low with respect to the accreted mass? • Advection vs. Outflows • What is the physics of Radio-Loud high accretion rate systems (QSOs)? • What fraction of the power do the most powerful jets carry? • How common are they (lifetime of the radio active phase)?

  6. Open questions in accretion theory • Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005)Þ jets/outflows dominate over radiation as power sinks. But is radiative efficiency low with respect to the accreted mass? • Advection vs. Outflows • What is the physics of Radio-Loud high accretion rate systems (QSOs)? • What fraction of the power do the most powerful jets carry? • How common are they (lifetime of the radio active phase)?

  7. Compact radio jets “Jet line” Transients GX 339-4 (2002/03 outburst) Belloni and Homan (2005)

  8. Scaling relations and the low/hard state • Compact, self-absorbed synchrotron emission from the jet core • 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 • The observed radio-X-ray correlation (LR~LX0.7) implies: • X-ray emission is radiatively inefficient (LX~Mdot2) • LKin ~ LR1.4 Heinz and Sunyaev 2003; Merloni et al 2003; Heinz 2004

  9. Scaling relations and the low/hard state • Compact, self-absorbed synchrotron emission from the jet core • 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 • The observed radio-X-ray correlation (LR~LX0.7) implies: • X-ray emission is radiatively inefficient (LX~Mdot2) • LKin ~ LR1.4 Heinz and Sunyaev 2003; Merloni et al 2003; Heinz 2004

  10. A0620 in quiescence: a unique tool No evidence for break in correlation down to about 10-9 LEdd Gallo et al. 2006

  11. Eoutburst ~ 2-4 ´ 1044 ergs Ejet,Q ~ 5 ´ 1044 W ergs A0620 in quiescence: does the jet take all? • The radiative inefficiency of the source (from comparing outer accretion rate with luminosity) and the slope of LR-LX correlation imply (Merloni, Heinz and Di Matteo 2003) Gallo et al. (2006); Heinz and Grimm (2005)

  12. Accretion diagram for LMXB (Blandford & Begelman 1999)

  13. What about radio galaxies and AGN? • Verify the hypothesis that AGN at low luminosity release most of their power as Kinetic Energy and the Low-hard state scaling • Need independent measures of LKin and LR (and/or LX, MBH) • Dynamical, from models of jet/lobe emission and evolution • Cyg A, M87, Perseus A • Indirect, from estimates of PdV work done on sourrounding gas (X-ray cavities) (Allen et al. 2006; Rafferty et al. 2006)

  14. Core Radio/X-ray correlation in AGN Open triangles: BH binaires Closed squares: AGN LR/LEdd1.4 5LX/LEdd Merloni et al. 2003; Maccarone et al. 2003.

  15. What about radio galaxies and AGN? • Verify the hypothesis that AGN at low luminosity release most of their power as Kinetic Energy and the Low-hard state scaling • Need independent measures of LKin and LR (and/or LX, MBH) • Dynamical, from models of jet/lobe emission and evolution • Cyg A, M87, Perseus A • Indirect, from estimates of PdV work done on sourrounding gas (X-ray cavities) (Allen et al. 2006; Rafferty et al. 2006)

  16. Core Radio/LKin correlation in AGN Cyg A, Carilli & Barthel ‘97 Allen et al. 2006 Rafferty et al. 2006 Per A, Fabian et al. 2002 M87, Bicknell & Begelman ‘96 Lkin=6×1037(LR/1030)0.7 Merloni & Heinz, in prep.

  17. The Kinetic Luminosity Function of AGN • Derive the intrinsic, un-beamed core radio luminosity function of AGN from the observed flat spectrum radio sources LF (Dunlop & Peacock 1990). • Assumes radio jets have all the same Gamma factor (or a distribution peaked around a single value) • Use the LR/LKin relation to estimate kinetic power in low state objects • Assume that 10% of high state objects are radio loud with Lkin~Lbol (Merloni 2004; Heinz, Schwab & Merloni 2006; Merloni et al. 2006)

  18. The Kinetic Luminosity Function of AGN Merloni & Heinz, in prep.

  19. Kinetic Luminosity Function of AGN: Evolution • Estimate accretion rate onto the black hole and kinetic energy output for any given LR-LX-MBH combination • Solve continuity equations for BH growth (Small and Blandford 1992; Marconi et al. 2004) backwards in time, using the locally determined BH MF as a starting point (Merloni 2004; Heinz, Schwab & Merloni 2006; Merloni et al. 2006)

  20. Kinetic Energy output and SMBH growth Merloni & Heinz, in prep.

  21. Kinetic Energy output and SMBH growth Merloni & Heinz, in prep.

  22. Energy budget ~ 83-90 % ~ 9-16 % ~ 4-11 % ~ 2-3 % Kinetic Energy output and SMBH growth Merloni & Heinz, in prep.

  23. Conclusions • Constraints on the physics of accretion/jet production are crucial for our understanding of feedback • “Low-luminosity AGN” are most likely dominated by kinetic energy as a sink of energy • Physically motivated scaling Lkin ~ Lcore,5GHz0.7 • The redshift evolution of SMBH mass, accretion rate and kinetic energy output function can be determined from the joint evolution of X-ray and Radio AGN luminosity functionsusingthe mass-LX-LR relationship • The K.E. feedback from LLAGN jets at late times starts dominating high mass objects first and then objects of progressively lower mass (downsizing of feedback) • The occurrence of the so-called “radio mode” of AGN feedback is in fact only determined by accretion physics

  24. The M87 jet Hubble Heritage Project http://heritage.stsci.edu/2000/20/index.html

  25. giant radio flares Compact radio jets Transient Black Hole Accretion “Jet line” GX 339-4 (2002/03 outburst) Belloni and Homan (2005)

  26. A0620-00 (V616 Mon) • In 30 years, IR/Optical/UV campaign have revealed system parameters to a high level of accuracy: • D = 1.2 ± 0.4 Kpc • M = 11.0 ± 1.9 M๏ • 0.7M๏ K3-K4V companion in a 7.75 hr orbit • Optical accretion disc spectra and total energy released in outburst have been used to estimate the outer disc accretion rate of ~1-3 × 10-10 M๏ /yr (about 5 orders of mag. larger than that onto BH if accretion efficient;McClintock et al. 1995; Meyer-Hofmeister & Meyer 1999)

  27. 2005 campaign: X-ray radio observations • 2-10 keV Luminosity (D=1.2 kpc) • LX=7.1+3.4-4.1 x 1030 erg/s Radio Flux density 51.1 μJy/beam (7.3σ) Lowest reported for an X-ray binary so far LR=7.5±3.7 × 1026 erg/s

  28. On the origin of radio emission • Typical radio luminosities of early-to-mid type K stars is in the range 1 × 1014 up to 3× 1015 erg/s/Hz (factor of 30 smaller than what observed in A0620-00) • Unlikely optically thin radio flare, seen at much larger (outburst) luminosity and/or larger scales • Free-free emission unlikely, as would imply too large mass loss • ADAF predictions fall short by more than 3 orders of magnitude • Likely, continuous, persistent relativistic outflow with flat spectrum as seen in low/hard state sources

  29. Accretion theory in a nutshell (Blandford & Begelman 1999)

  30. Accretion theory in a nutshell

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