1. Accretion in Early-Type Galaxies Haiguang Xu Department of Physics Shanghai Jiao Tong University hgxu@sjtu.edu.cn

2.  Acrretion from the ambient cosmological flow – origin of the ISM – gas heating  Accretion by a central massive black hole – central engine of an AGN – jet and heating of the ISM  Accretion by an intermediately massive black hole in globular clusters – intermediate mass black holes – ULXs – formation and evolution of AGNs

3. 1 Central Source Host galaxies of the radio–loud quasars and radio galaxies appear to be giant elliptical galaxies  Existence of central massive black holes e.g., a few 10 7 M  in N4472, 10 8–9 M  in quasars (Wu et al. 2003)  The continuing accretion of the hot gas from the extensive halo should make these galaxies more luminous than they appear if the radiative efficiency is 10% (e.g., Fabian & Canizares 1988) Bondi Accretion: > 10 43 erg s –1 in most giant ellipticals (e.g., Fabbiano 1989) Total X-ray luminosity in E galaxies: 10 36–43 erg s –1, diffuse & point sources the problem of starving the monster  Lower accretion rate?  Lower radiative efficiency? Fabian & Rees 1995

4. Possible solutions (e.g., Fabian & Canizares 1988, Nature 333, 829)  Emissions in unobservable bands  Kinetic energy in the jet  Outflows or relativistic gas surrounding the BH that preventing accretion  Angular momentum that preventing the gas from reaching the BH  Time dependnce  Low efficiency  Most bright elliptical galaxies do not contain massive black holes

5. NGC 6166 (Abell 2199) Di Matteo et al. 2001  Central black hole:  10 9 M   Bondi rate: < 3  10 –2 M  yr –1 about 10 times lower than the ROSAT HRI values for e.g., M87, NGC 4649 & NGC 4472 (Di Matteo et al. 2000), but more consistent with high frequency radio measurements (Di Matteo et al. 1999, 2000; Wrobel & Herrnstein 2000)  A nuclear luminosity of  10 44 erg s –1 in X-rays if the radiative efficiency is 10%, which is 4 orders of magnitudes larger than the Chandra measurement in 0.5–7 keV (4  10 40 erg s –1 )   = 10 –5 pure inflow ADAF models are preferred (e.g., Rees et al. 1982) However, the Bondi accretion rate may have been overestimated, and the requirement for low radiative efficiency may be relaxed, because  Gas density and temperature are measured at about 1 kpc (15 R A )  If strong convection develops, as in CDAFs, accretion rate could be reduced  Heating of the ISM by the jets could decrease the Bondi accretion radius

6. M87 (Virgo) Di Matteo et al. 2003 Spatial resolution of Chandra: < 100 pc (a few 105 Schwarzschild radii)  Central black hole: 3  10 9 M  (e.g., Ford et al. 1995; Harms et al. 1995)  Bondi rate:  0.1 M  yr –1 L Bondi = 5  10 44 erg s –1 with  = 0.1  L 0.5-7 keV = 7  10 40 erg s –1  Multiwavelength spectrum of the nucleus is consistent with the prediction of a advection dominated flow  The flow shall be modified by the existence of jet and/or outflow Most of the accretion energy is released in the relativistic jet that may reduce the accretion rate. The central engine may undergoes on-off activity circles Chandra 0.5-5 keV

7. NGC 1399, NGC 4472, NGC 4636 Loewenstein et al. 2001 NGC 4636

8.  For 10 8–9 black holes, the observed upper limits of the luminosity are 7.3  10 –9 L Edd (NGC 1399) 15  10 –9 L Edd (NGC 4472) 28  10 –9 L Edd (NGC4636)  so that the corresponding radiative efficiencies of Bondi accretion are extremely low 4.1  10 –6 (NGC 1399) 24  10 –6 (NGC 4472) 620  10 –6 (NGC4636) These are inconsistent with the standard advection-dominated accretion flow models for NGC 1399 and NGC 4472  Accretion rates at lower than 10% of the Bondi rate Faint soft central sources in NGC 4472 & NGC 4649 (Soldatenkov et al. 2003) Detectedable below 0.6 keV, heavily absorbed 0.2–2.5 keV luminosity: 1.7  10 38 erg s –1 for NGC 4472 6  10 37 erg s –1 for NGC 4649

9. 2 Black Holes in Globular Clusters A tight correlation between the mass of a galaxy’s central black hole and the luminosity-weighted line-of-sight velocity dispersion within the half-light radius for 26 galaxies (Gebhardt et al. 2000)  The formation process of both bulges and massive clusters is similar (Gebhardt et al. 2000) Gas Kinematics Stellar Kinematics Maser Dtections

10. A 2.0(+1.4, –0.8)  10 4 M  Black Hole in G1 (M31) Gebhardt et al. 2002 A 3.9(±2.2  10 3 ) M  Black Hole in M15 Gerssen et al. 2002  But see Naccarone et al. 2005: uppers limit of about 100  Jy at GHz frequencies  < 100 M  with Bondi-Hoyle rate with an upper limit of about 1000 M  if more realistic assumptions are made by using a larger accretion rate G1 (M31)

11. Gebhardt et al. 2002

12. Zheng 2001

13. Chandra Study of NGC 4552 47 LMXBs 25 LMXBs and 210 GCs In the 4 Re region of NGC 4552  47 X-ray point sources; central source: 4  10 39 erg s –1 not very soft, no excess absorption  of the 46 off-center sources, 3 have luminosities > 10 39 erg s -1 1 is associated with a GC and has M=15–135 M 

14. Chandra Study of NGC 1407

15. X-ray point sources with L X > 10 39 erg s -1 in NGC 1407 kT in (keV)L X (10 39 erg s –1 )Mass (M Sun ) (Schwarzschild) Mass (M Sun ) (Kerr) 0.371.088960-536 0.681.753422-202 1.272.01106.7-60 0.493.699463-566 1.061.921510-87 2.172.083.62.4-22

16. A Radio Test of the Existence of Intermediate Mass Black Holes in Globular Clusters and Dwarf Spheroidal Galaxies Maccarone 2004

17. ULXs and Formation of IMBHs 1) The accreting black holes have ordinary stellar mass whose emission is beamed (King et al. 2001) 2) These black holes formed directly via evolution of Popular III stars (Madau & Rees 2001) 3) These black holes grow by accretion (Miller & Hamilton 2002) The Accretion Scenario  A black hole with < 10 3 M  accreting from the ISM  too slow  A 10 M  black hole sinks to the cluster core within 10 7 yr to form a binary, which is tightened by 3-body interactions that cause recoil  kickout (Sigurdsson & Hernquist 1993)  Growth from a > 50 M  black hole in 10 10 yr

18. Kawakatu & Umemura 2005

19. 3 X-Ray Luminosity Function of Point Sources NGC 4697 Sarazin et al. 2000 A knee on the XLF around the Eddington Luminosity of normal accreting neutron stars with a mass of 1.4 M , L Edd = 2  10 38 erg s –1 Also in NGC 1553 (Blanton et al. 2001) NGC 4472 (Kundu et al. 2002) However, for a sample of 14 E/S0 galaxies, Kim and Fabbiano (2004) found the break is higher. NGC 720 (Jeltema et al. 2003), NGC 4365, NGC 4382 (Sivakoff et al. 2003) M87, M49, M4697 (Jordan et al. 2004): a break/cutoff at > 10 39 erg s –1 NGC 1600 (Sivakoff et al. 2004): no break

20. The Cumulative X-Ray Luminosity Function of NGC 1407 Zhang et al. 2005  A broken power-law profile with L b =4.4  10 38 erg s -1  No obvious difference between the luminosity distributions of GC LMXBs and field LMXBs.