5GHz, VLA image of Cyg A by R. Perley

Cosmological growth of SMBH:Cosmological growth of SMBH:the kinetic luminosity function of AGNthe kinetic luminosity function of AGN

IAU Symposium 238IAU Symposium 238 – PraguePrague 22/08/200622/08/2006

Andrea MerloniMax-Planck Institute for Astrophysics

&Sebastian Heinz

MIT

• 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

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

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

Intro: Key questions

• Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005) 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)?

Open questions in accretion theory

• Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005) 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)?

Open questions in accretion theory

“Jet line”

Belloni and Homan (2005)

GX 339-4(2002/03 outburst)

Compact radio jets

Transients

Heinz and Sunyaev 2003; Merloni et al 2003; Heinz 2004

• 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

Scaling relations and the low/hard state

Heinz and Sunyaev 2003; Merloni et al 2003; Heinz 2004

• 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

Scaling relations and the low/hard state

No evidence for break in correlation down to about 10-9 LEdd

Gallo et al. 2006

A0620 in quiescence: a unique tool

• 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)

Ejet,Q

~ 5 1044 W ergs

Eoutburst

~ 2-4 1044 ergs

Gallo et al. (2006); Heinz and Grimm (2005)

A0620 in quiescence: does the jet take all?

(Blandford & Begelman 1999)

Accretion diagram for LMXB

• 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)

What about radio galaxies and AGN?

Core Radio/X-ray correlation in AGN

5LX/LEdd

LR/LEdd1.4

Merloni et al. 2003; Maccarone et al. 2003.

Open triangles: BH binairesClosed squares: 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)

What about radio galaxies and AGN?

Merloni & Heinz, in prep.

Core Radio/LKin correlation in AGN

Cyg A, Carilli & Barthel ‘97

Per A, Fabian et al. 2002

M87, Bicknell & Begelman ‘96

Allen et al. 2006

Rafferty et al. 2006

L kin=6×1037 (L R

/1030 )0.7

• 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)

The Kinetic Luminosity Function of AGN

The Kinetic Luminosity Function of AGN

Merloni & Heinz, in prep.

• 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)

Kinetic Luminosity Function of AGN: Evolution

Kinetic Energy output and SMBH growth

Merloni & Heinz, in prep.

Kinetic Energy output and SMBH growth

Merloni & Heinz, in prep.

Kinetic Energy output and SMBH growth

Energy budget

~ 83-90 %

~ 2-3 %

~ 9-16 %

~ 4-11 %

Merloni & Heinz, in prep.

• 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 functions using the mass-L

X-L

R

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

Conclusions

The M87 jetHubble Heritage Project

http://heritage.stsci.edu/2000/20/index.html

Transient Black Hole Accretion

Belloni and Homan (2005)GX 339-4

(2002/03 outburst)

“Jet line”

giant radio flares

Compact radio jets

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๏

• 0.7 M ๏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)

2005 campaign: X-ray radio observations

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

–2-10 keV Luminosity (D=1.2 kpc)

–LX=7.1+3.4-4.1 x 1030 erg/s

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

(Blandford & Begelman 1999)

Accretion theory in a nutshell

Accretion theory in a nutshell