1. Almost every galaxy hosts a BH 99% are silent 1% are active 0.1% have jets Extragalactic jets: a new perspective G. Ghisellini in coll. with F. Tavecchio INAF-OABrera

2. FRI-FRII & Blazars

3. Synchro Inverse Compton (also possible hadronic models) Radio IR Opt UV X MeV GeV Blazars: Spectral Energy Distribution

4. Fossati et al. 1998; Donato et al. 2001 The “blazar sequence” FSRQs BL Lacs LBL and HBL

5. Fossati et al. 1998; Donato et al. 2001  peak B 2

6. By modeling, we find physical parameters in the comoving frame.  peak is the energy of electrons emitting at the peak of the SED EGRET blazars TeV BL Lacs

7. Low power slow cooling large  peak Big power fast cooling small  peak

8. Power of jets in blazars …and X-ray cavities, Allen+, 2006, Balmaverde+, 2008

9. Power of jets in blazars Tavecchio+ 2000 Celotti, GG 2001

10. Power of jets in blazars

11.  P r = radiation P e = relat. electrons P p = protons P B = B-field R The power of blazar jets R diss ~10 17 cm

12. Ghisellini, Foschini, Tavecchio, Pian 2007 AGILE! 3C 454.3 Swift

13. If one p per e- Relat. electrons Magnetic Field Radiation Celotti & Ghisellini 2007 High power P o w e r f u l j e t s a r e n o t m a g n e t i c a l l y d o m i n a t e d Celotti GG 2008

14. Celotti GG 2008, Maraschi et al. 2008 P jet 10x 100x

15. Disk accretion rate (Eddington units) L disk P jet L disk P jet Jet power vs disk Lum. e-p decoupling Photon trapping BL Lacs, FSRQ,  QSO GRBs

16. Pause Jet power is large. More than L diskJet power is large. More than L disk Matter dominated. Not many pairsMatter dominated. Not many pairs P B is smallP B is small Powerful jets must be radiatively inefficientPowerful jets must be radiatively inefficient Powerful jets do not deceleratePowerful jets do not decelerate

17. A new blazar sequence Old one: based on 1 parameter: the observed luminosity Now: info on mass and accretion rate (spin? not yet) Info on jet power vs disk luminosity Info on location of dissipation: must be at some distance from BH. One zone is dominant (internal shocks?)

18. The key ideas R diss proportional to M BH R BLR proportional to (L disk )  U BLR =cost For L disk /L Edd < L c  no BLR (BL Lacs) 1/2

19. Ledlow & Owen Ghisellini & Celotti 2001

20. The key ideas R diss proportional to M BH R BLR proportional to (L disk )  U BLR =cost For L disk /L Edd < L c  no BLR (BL Lacs) P B =  B P jet  B propto R -1 P e =  e P jet 1/2

21. P B =  B P jet  B propto R -1 P e =  e P jet Celotti & Ghisellini 2008

22. The key ideas R diss proportional to M BH R BLR proportional to (L disk )  U BLR =cost For L disk /L Edd < L c  no BLR (BL Lacs) P B =  B P jet  B propto R -1 P e =  e P jet   peak propto U -1 ; U -1/2 1/2

23. The key ideas R diss proportional to M BH R BLR proportional to (L disk ) For L disk /L Edd < L c  no BLR (BL Lacs) P B =  B P jet P e =  e P jet   peak propto U -1 ; U -1/2 The key ansatz P jet always proportional to M 1/2

24. M2 M2 M2 M2 M ADAF (Narayan et al.) P jet propto L disk 1/2

25. Simple consequences R diss propto M; R BLR propto (L disk ) 1/2R diss propto M; R BLR propto (L disk ) 1/2 BLR Low M, High L disk  Red quasar High M, Low L disk  Blue quasar

27. Simple consequences Small M, small P jet, large B, redSmall M, small P jet, large B, red BLR U BLR ~ the same Large U B

29. Synchrotron peak frequency

30. Inverse Compton peak frequency

31. Compton dominance

32. Give me M BH and L disk (or L BLR ) and I will tell you the SED of the jet and its power Reproducing the “old” sequence

33. Conclusions P jet > L diskP jet > L disk Jets are matter dominatedJets are matter dominated Link between M, M and observed SEDLink between M, M and observed SED “Blue” FSRQs may exist“Blue” FSRQs may exist “Red” low power FSRQs may exist“Red” low power FSRQs may exist Implications about evolutionImplications about evolution GLAST + Swift + M + L disk (or L BLR )GLAST + Swift + M + L disk (or L BLR )

34. Fossati et al. 1998; Donato et al. 2001 AGILE GLAST CT Swift