1. Multi-wavelength emission models in blazars Gabriele Ghisellini INAF-Osservatorio di Brera with A. Celotti, R. Della Ceca, L. Foschini, G. Ghirlanda, F. Haardt, L. Maraschi, G. Pareschi, T. Sbarrato, G. Tagliaferri, F. Tavecchio, M. Volonteri

2. BL Lacs vs FSRQs: the blazar sequence

3. Fossati et al. 1998; Donato et al. 2001 The “blazar sequence” FSRQs BL Lacs BATIntegral

4. FSRQs Line strength Fossati et al. 1998; Donato et al. 2001

5. FSRQs BL Lacs M/M Edd Fossati et al. 1998; Donato et al. 2001 Next talk by Meyer

6. 3 months, 10 

7. Blazars: the redder the more powerful  cooling GRBs: the bluer the more powerful  heating??  ? “Amati” “Ghirlanda” E peak [keV] E [erg]

8. Jet-accretion connection & location

9. Sbarrato+ 2011 SDSS+1LAC Do we really need to divide blazars? 5x10 -4 EW<5A EW>5A Narayan & Yi 1995: L BLR /L Edd ~ 10 -3 Sharma+ 2007: L BLR /L Edd ~ 10 -5 M-  Plotkin+ 2011

10. Torus ~1-10 pc Broad Line Region ~0.2 pc Within R BLR U BLR = const Within R Torus U IR = const  R BLR R Torus disk Big blazars Poutanen L>0.01L Edd Sikora Leptonic view. For adronic: next talk by Boettcher  T ~   HeII

11. Torus ~1-10 pc Broad Line Region ~0.2 pc ~VLBI region ~20 pc away (Marscher+)  R BLR R Torus disk Lyutikov Also Joshi, next talk L>0.01L Edd

12. TeV X TeV BLR <<0.2 pc weak cooling SSC only “ADAF disk”  L<0.01L Edd

13. Black hole masses (for FSRQs)

14. UVOT XRT Fermi GG, Tavecchio & Ghirlanda 2009 Low energy synchro peak: leave the disk naked! torus disk X-ray corona synchro SSC EC  M BH =2x10 9

15. GG, Tavecchio & Ghirlanda 2009 torus disk X-ray corona synchro SSC EC Small B M BH =2x10 9

16. BAT M BH =10 10

17. Jet power

18. The jet cannot have less power than what required to produce the observed luminosity: P jet L obs 2222 > If P jet is twice as much,  halves. We can take that as the minimum P jet. This limit is model-independent.

19.   

20. 1 proton per electron  no pairs Having pairs would reduce P jet. But where are they created?

21. Pairs and radio-galaxies

22.  We cannot produce pairs here!!

23.  Efficient pairs production if primary spectrum peaks at ~MeV

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

25. Two epochs of heavy BH formation?

26. Recently, two complete surveys of blazars: BAT and LAT (Ajello+2009, 2012). BAT has fewer blazars, but more at high redshifts. All BAT blazars at z>2 have M BH >10 9 M 0. These all have L x > 10 47 erg/s and L disk > 0.1 L Edd

27. GG+2010, Volonteri+ 2012; GG+ 2013 Heavy & Active: M > 10 9 ; L disk > 0.1 L Edd

29. Hopkins+ 2007 Two epochs of formation of massive BH? Radio-loud: z~4 Radio-quiet: z~2

30. Jets  spin  high accretion efficiencies  slow growth

31. It takes too long! Eddington accretion starting at z=20

32. Jets for all M/M Edd Location is an issue Look if radio-galaxies peak at ~1 MeV with L~10 45 erg/s Heavy BH in jetted AGNs form earlier Jets & Spin? Something must be changed Conclusions