1. Active galaxies / Active galactic nuclei (AGN)
Central engine
variability put limit on size: R ≤ c var
Schwarzschild radius: Rs = 2 G M / c2
Rs = size approx Uranus orbit for 109 M
Accretion allows conversion of 0.1mc2
(fusion only 0.7%)
Radiation pressure will larger than gravity if L > LEDD
Accretion disk very hot continuum source => X-rays
Broad line region, dense ionised clouds, rapid moving
Narrow line region, dilute ionised clouds, slower
reverbration mapping
Obscuring torus with dust and molecular gas,
sublimation evacuate central part -> torus
Relativistic (superluminal) Jets, and radio Lobes

3. Unified AGN models Idea: all AGN are basically the same phenomena
Differing due to different viewing angle and scale:
Face on view: see all components: Sy1, QSO
if looking into jet: Bl Lac (Blazar)
Edge on view: see only hot torus and NLR, Sy2
Why some radio loud while others not?
Unified BH model not perfect, but nothing else works

4. Unified Model

5. Spiral seyfert2 with radio jets

6. QSO evolution - where are they now?
Debate if fall off
at z>3 is real
There must be many dead QSOs around in the local universe!

7. Kinematical evidence for BH in M87
+ Grav redshifted X-ray em-lines detected in Sy1’s

9. Relation between black hole mass and sigma of host
galaxy: a realtion between BH and Spheroid Mass
-- Black Hole doesn’t care about disk
-- Co-evolves with spheroid/bulge!

10. Clusters And Large Scale Structure (chapt. 4)

11. M33
LeoI
Sex A

13. Tidal drag on NGC205 from M31

14. Local Group

15. HCG31
Galaxy
Evolution/
Transformation
Caught in
action

16. Rich clusters: Virgo and Coma irregular vs regular
(large spiral fraction) (mostly ”early” types))
(more relaxed)

17. Hot gas in clusters X-ray emitting through thermal bremsstrahlung
Efficient way of finding
clusters

18. Butcher-Oemler effect, etc:
As we look back in time, the spiral fraction of
Rich clusters become higher and higher (BO)
Cluster and Galaxy transformation
Interactions: galaxy mergers
cluster merger
galaxy harassment
ram pressure stripping
diffuse intracluster light: stars + gas
vs Hot intracluster gas

19. Masses of clusters: Virial theorem: M = RA v2 / G - does it apply?
X-ray gas in Hydrostatic equilibrium does it apply?
Gravitational lensing:
it does apply but only gives mass contrast
- Methods agree fairly well (factor of 2)

20. Gravitational lensing

21. Einstein ring

22. Abell 2218, strong lensing cf weak lensing (statistical)

23. Angular distribution of Abell-clusters
Brightest cluster galaxy method allows
rough space distribution to be inferred

24. Virgo supercluster
Bound?
-Not relaxed
LargeScale
Flows

25. Sponge-like topology of universe
CfA
Redshift
Survey
Great wall
Voids!
Finger of god

26. SDSS

27. Intergalactic matter

31. Gunn-Peterson effect

32. Cosmic shear Challenging! - Effect on each individual galaxy tiny
- Only visible through lareg and deep samples

33. Measuring Clustering
- Count in cells
- 2-point corellation function