1. THE MODERATELY LARGE SCALE STRUCTURE OF QUASARS
Jari Kotilainen (Tuorla Observatory)

2. HIGH Z QUASARS AND GALAXY FORMATION
High z quasars: lighthouses of sites of galaxy formation
quasar space density vs BH growth rate vs SFR history
=> mergers trigger both SF and quasar activity?
=> rapid decline of BH activity at low z
Merloni et al. 2005

3. BHs in all (?) local massive bulges
Milky Way: M ~3 x 106 Msun
=> all massive galaxies host a remnant BH from a quasar phase?

4. tight MBH – Mbulge – σbulge correlations (at low z)
Kormendy 2004
tight MBH – Mbulge – σbulge
correlations (at low z)
masers gas stars
nearby quasar hosts: massive bulge-dominated galaxies

5. The most distant quasar (z = 6.4):
molecular gas, dust, SF, metals and BH
Barth et al. 2003
How did massive bulges and SMBHs form in < 1 Gyr?

6. QUASAR HOSTS AT HIGH REDSHIFT (z > 1)
Kotilainen et al ApJ 660, 1039
Falomo et al ApJ, in press
VLT + ISAAC non-AO imaging => 30 hosts at 1 < z < 2
VLT+NACO AO imaging =>
two RLQ hosts (z ~2.5 and z ~2.9) two RQQ hosts (z ~2.1 and z ~2.5)

7. Evolution of quasar host luminosity
RLQ hosts ~10 x more luminous (massive)
BH mass? mass accretion rate?
BH mass threshold for radio activity?
c.f. clustering properties, SEDs
RLQ
passive evolution into local massive spheroids
no decrease in luminosity ?
=> early epoch for the latest merger
decrease in luminosity ?
=> tight quasar - host co-evolution
different for RLQs and RQQs ?
RQQ

8. c.f. hierarchical structure formation…
… where BHs are fuelled and galaxies grow by mergers
=> predict decrease in host luminosity
=> NOT observed up to z = 2
Di Matteo et al. 2005
more recent models: AGN/SN feedback
Granato et al. 2004, Bower et al. 2006

9. WORK IN PROGRESS... evolution of MBH – Mbulge relation with z?
spectra of resolved quasars at 1 < z < 3
images => Mbulge spectra => virial MBH
z = 1.8
z = 2.5

10. MORE WORK IN PROGRESS...
CDM => massive density peaks in early Universe are strongly clustered: cores of rich clusters => clustering of high z quasars
for radio galaxies: threshold DM halo (BH) mass required to produce significant radio emission...
Magliocchetti et al. 2005

11. ...but no radio luminosity dependence of clustering/DM content/BH mass
Magliocchetti et al. 2005
also: lensing, close companions...
Falomo et al. 2005