1. The Links Between AGN and Galaxy Formation
Omar Almaini
University of Nottingham

2. The Links Between AGN and Galaxy Formation
Galaxy formation models
…and their problems
The AGN/galaxy connection
Feedback and AGN winds
Observing black hole/bulge growth
Summary & future prospects

3. CDM cosmological model in excellent agreement with wide range of observations:
e.g. CMB, galaxy clustering, type 1a SN, element abundances, Cepheid distance scale, stellar ages, baryon fraction in clusters…

4. Merger Tree for the Growth of a Dark-matter Halo

5. Semi-analytic Galaxy Formation Models+
Messy physics
(gas cooling, star-formation,
dust, SN feedback etc…)
N-body merger trees =

6. Hierarchical Galaxy Formation

7. Producing the local K-band luminosity function
-SN feedback is essential!
Benson (2003)

8. >5x1049 erg per solar mass required
Problem can be solved with extreme super-winds
>5x1049 erg per solar mass required
Benson (2003)

9. Local galaxies are strongly bimodal
Kauffmann et al. 2003; Balogh et al. 2004

10. Can’t make enough red galaxies at z>1
Data
Model
e.g. Daddi et al. 2002; Roche, Almaini et al. (2002),
Roche, Dunlop & Almaini (2003); Somerville et al. (2003)

11. The diversity of ERO galaxies
30-40% old, passive systems
30-40% dusty starburst
Typical redshifts 1.0<z<1.5
Strongly clustered
High space density
Many old, massive systems
already in place at z~1-1.5

12. ‘EROs’ at higher redshift
Recent discovery of many
old, passive systems at
z>1.5
Using J-K>2 colour selection
find population of very red
galaxies at z>2
Cimatti et al. 2004
Glazebrook et al. 2004
Van Dokkum et al. 2003

13. Summary of galaxy formation problems
Classic Problems
Predicts too many dwarf gals
Predicts “cuspy” cores
Why are there no galaxies
with  > 300 km/s?
Newer Problems
Fail to produce EROs
Fails to predict SCUBA sources
Bimodal local galaxy pop.
Need a mechanism for switching off
star-formation in most massive galaxies

14. II. The AGN/galaxy connection

15. All massive galaxies contain a SMBH

16. The black-hole/bulge mass relationship.
MBH = 1.5x108 2004 M
MBH = 0.2 % Mbulge
Gebhardt et al. (2000), Ferrarese & Merritt (2000)
c.f. Magorrian (1998)

17. Ebulge ~ Mbulge 2 ~ 10-6 Mbulge 2300 c2
Can the black hole influence its host galaxy?
MBH = 2x10-3 Mbulge
AGN radiative energy
EAGN ~ 0.1 MBH c2
= 2 x Mbulge c2
Binding energy of the bulge
Ebulge ~ Mbulge 2
~ 10-6 Mbulge 2300 c2
Less than 1% of the AGN energy could blow the galaxy apart

18. The X-ray background: Most accretion activity is absorbed
Unobscured AGN

19. “AGN winds are ubiquitous” - Brad Peterson
“My wind model explains everything” - Martin Elvis

20. APM-08279 – lensed BAL quasar at z=3.91
Fe XXV K ?
v1~0.2 c
v2~0.4c
Chartas et al. (2002)

21. Massive X-ray outflow in PDS 456
XMM EPIC pn/MOS
Reeves et al. (2003)

22. Massive X-ray outflow in PDS 456
XMM RGS-2
V~50,000 kms-1
NH = 5x1023
~ 10 M yr-1
Momentum outflow:
Mwind v ~ L Edd/c .
Reeves et al. (2003)

23. Investigated supercritical accretion
King & Pounds 2003
Investigated supercritical accretion
M > M Edd . . ~
Assuming all excess matter ejected in a wind:
Compton-thick, quasi-spherical outflow
Momentum outflow: .
Mwind v ~ f L Edd/c

24. Blandford 1999, Di Matteo et al. 2004… )
King 2003
(c.f. Silk & Rees 1998, Fabian 1999,
Blandford 1999, Di Matteo et al. 2004… ) .
Momentum outflow:
Mwind v ~ L Edd/c
Outflow drives wind bubble through host galaxy
M(R)  2 R
Mgas(R)  2 R
Shell velocity v2  Ledd / 2
MBH  4

25. The black-hole/bulge mass relationship.
MBH = 1.5x108 2004 M
MBH = 0.2 % Mbulge
Gebhardt et al. (2000), Ferrarese & Merritt (2000)
c.f. Magorrian (1998)

26. Observations of AGN-driven super- winds now required!

27. A cartoon model of massive
galaxy formation
SCUBA phase
quasar
elliptical?

28. II. AGN in galaxy clusters

29. The Entropy Problem (SN not enough?)

30. The Cooling-Flow Problem
XMM RGS (Virgo)
Sakelliou et al. 2002

31. Chandra
VLA

33. II. Observing joint black-hole/ galaxy formation

34. What is so special about submm sources?
fn
The James Clerk
Maxwell Telescope
(Hawaii)
1000
100 10
Wavelength / m

35. Results of submm surveys
Highly luminous (ULIRG) systems
SFR ~ 1000 M yr-1
Massive systems
Evidence for outflowing winds
Progenitors
of massive
elliptical galaxies?

36. Mass determinations for submm sources
Genzel et al. (2003)
Swinbank et al. (2004)
Massive (CO)
Massive (Ha)

37. Semi-analytic models have great difficulty producing submm sources…
Baugh et al. (2005)

38. Most SCUBA sources DO NOT contain powerful quasars
Almaini et al. 2003

39. William Herschel Telescope 4m
5 "
William Herschel Telescope 4m
Depth R~27 Seeing 0.7”
5 "

40. HST ACS Imaging – (Almaini et al. 2005)
5 "
HST ACS Imaging – (Almaini et al. 2005)

41. 1.945 Ms “True” color image ACIS-I exposure P.I.: W.N. Brandt
keV keV keV
P.I.: W.N. Brandt

42. P.I.: W.N. Brandt Alexander et al. 2005
1.945 Ms
ACIS-I
exposure
“True” color image
keV keV keV
P.I.: W.N. Brandt
17/20 SCUBA galaxies
X-ray detected
Alexander et al. 2005

43. Joint spectral fitting
Composite 2-20 keV spectra (12Ms)
Joint spectral fitting
12Ms Chandra spectra!

44. Relatively low Lx/LFIR ratios

45. Evidence for growing black holes?
1.945 Ms
ACIS-I
exposure
“True” color image
keV keV keV
P.I.: W.N. Brandt
Modest X-ray luminosities
Lx = ergs-1
Suggest black holes <108M
Alexander et al. 2005
Evidence for growing black holes?

46. Eddington limited growth
Fuel supply
Eddington limited growth
Archibald et al. (2002)

47. Where do we go from here? Need detailed prescription for AGN
feedback in semi-analytic models.
Can we detect merging black holes
with LISA (Madau 2004)?
How prevalent are AGN-driven
winds?
How massive were first black holes?
What influence did they have on
the IGM at z>10?

48. Conclusions Overwhelming evidence for CDM
 hierarchical structure formation
Problems with semi-analytical galaxy formation models
- mechanism required to terminate SF in massive gals
- plus other problems…
AGN feedback is a likely solution
- may be related to the origin of the M/ relation
- could also explain high-mass cut-off & cluster
heating problem