THE MODERATELY LARGE SCALE STRUCTURE OF QUASARS

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 gt mergers trigger both SF and
quasar activity? gt 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
gt all massive galaxies host a remnant BH from a
quasar phase?
4
Kormendy 2004
tight MBH Mbulge sbulge 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 lt 1 Gyr?
6
QUASAR HOSTS AT HIGH REDSHIFT (z gt 1)
Kotilainen et al. 2007 ApJ 660, 1039 Falomo et
al. 2007 ApJ, in press

• VLT ISAAC non-AO imaging gt 30 hosts at 1 lt z lt
  2
• VLTNACO AO imaging gt
• 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 ? gt early epoch for
the latest merger decrease in luminosity ? gt
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 gt predict decrease in host luminosity gt
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 lt z lt 3
images gt Mbulge spectra gt virial MBH
z 1.8
z 2.5
10
MORE WORK IN PROGRESS...
CDM gt massive density peaks in early Universe
are strongly clustered cores of rich clusters gt
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 Magliocche
tti et al. 2005
also lensing, close companions...
Falomo et al. 2005