1. Properties of Blazars The “blazar sequence” BL Lacs FSRQs
Fossati et al. 1998; Donato et al. 2001
The “blazar sequence”
FSRQs
BL Lacs

2. 3 months, 10 s

3. Torus ~1-10 pc
BLR
Standard disk G
L>0.01LEdd

4. L<0.01LEdd SSC only weak cooling G TeV “ADAF disk” X TeV
BLR <<0.2 pc
weak cooling
SSC only
“ADAF disk” G
TeV

5. FSRQs
BL Lacs
FSRQs
BL Lacs
More secure
uncertain G G
Rdiss

6. G G

7. G G

8. G G

9. GROND + UVOT
Ly-a absorpt.  phot. z
Rau+ 2012
Padovani+ 2012

10. GG+ 2012

11. Jump!

12. GG+ 2012

13. GG+ 2012

14. Jet power
- Big
- How much? How many pairs?
- Matter dominated

15. Having pairs would reduce Pjet. But where are they created?
1 proton per electron  no pairs
Having pairs would reduce Pjet. But where are they created?

16. G
Efficient pairs production if primary spectrum peaks at ~MeV

17. If z=0.3

18. If z=0.3 Two goals: 1) reduce power
2) more energy to leptons, less to protons

19. out
in ~ 10 Rs, G~2
out ~ 103 Rs, G~12 in in
out
GG 2012 in
out

20. Conclusions Reasonable understanding (compare with GRBs…) Open issues:
Pjet even larger than Mc2?
dissipation region (in, out, or very far out?)
Extreme TeV (not touched here)
The Rs zone: a real or an apparent gap? M87?
The 1-3 Rs zone…. (the engine)
Spin? Blandford-Znajek?
In the near future:
CTA use TeV BL Lacs as probes – surprises?
High z blazars with large black hole masses: 1=2G2
Radio-galaxies peaking at 1 MeV?