1. Blazars & GRBs Gabriele Ghisellini INAF-Osservatorio di Brera The fastest macroscopic objects of the Universe

2. 

3. Lister+ 2013 ~10  > 10 Fermi FSRQs 

4. Earlier on: isotropic explosion

5.    Later: energy crisis + collapsar scenario

6.       jet Blazars: collimation 1/  GRBs: collimation GRBs: collimation  jet

7.       jet Blazars: collimation 1/  GRBs: collimation GRBs: collimation  jet

8.       jet L ~ L’  4 L ~ L’ (  jet ) 2 Blazars GRBs

9. 0 Molinari+ 2007

10. 0

11. 0  E k,iso n t peak 3 1/8 t peak

12. Ghirlanda+ 2012 Liang+ 2012

13. Blazars: the general picture

14. 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 L>0.01L Edd

15. BLR <<0.2 pc weak cooling SSC only “ADAF disk”  L<0.01L Edd BL Lacs

16.   R diss FSRQs: emission lines  many seed photons BL Lacs: no or weak lines

17. FSRQs BL Lacs  FSRQs  R diss FSRQs BL Lacs

18.   FSRQs FSRQsFSRQs

19. Blazars and GRBs: same efficiency

20. Collimation corrected Nemmen+ Science 2012 blazars GRBs

21. Fermi blazars, one p per e- GRBs

22. Jet launching Internal pressure or magnetic field? or magnetic field?

23.      n o R Jet opacity: blazars n o from M out     ~ 0.5 1 P jet 1 P jet  1 L Edd Jet opacity: GRBs aT 0 4 kT 0 ~ n +     ~ P jet,51 M1M1M1M1 10 15 1/23/4

24. Jet launching In GRBs we have 2 possibilities: - internal pressure: the huge optical depth traps photons inside - magnetic field In blazars: - internal pressure: the optical depth is small - magnetic field

25. Jet launching In GRBs we have 2 possibilities: - internal pressure: the huge optical depth traps photons inside - magnetic field In blazars: - internal pressure: the optical depth is small - magnetic field Magnetic field: - Produced and amplified by the disk - Link with accretion

26. Blandford & Znajek  U B ~  c 2 @ R s This explains why P j ~ L d B ~ 10 15 -10 16 G in GRBs B ~ 10 4 G in blazars B ~ 10 9 G in galactic superluminals

27. synchro EC Small B torusdisk X-ray corona

28. Fermi FSRQs Power in cold protons (1 per emitting e-) Power in rel. electrons Power in Poynting flux Power in radiation (model indipendent) Disk luminosity

29. M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars:

30. M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars:  P jet LdLdLdLd M out M in = ~ 10 -2 blazars

31. M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars: for GRBs: M in ~ 0.1 M O t burst  P jet LdLdLdLd M out M in = M out M in =  c 2 0.1 M O EkEkEkEk ~ 5.5x10 -4 2222 E k52 ~ 10 -2 blazars

32. Blazars and GRBs: a difference

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

34. Conclusions Jets are the most efficient engine of Nature Compare jet power and L disk as a function of the accretion rate. Normalize to Eddington.

35. 1644+57? Late prompt in GRBs?

37. blazars GBRs

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

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

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

43. 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

44. Black hole masses (for FSRQs)

45. 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

46. BAT M BH =10 10

47. 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.

48.   

49. 1 proton per electron  no pairs Having pairs would reduce P jet. But where are they created?

51. Pause P jet ~ Mc 2, even larger than L dP jet ~ Mc 2, even larger than L d For all M/M EddFor all M/M Edd BL Lacs  ADAF FSRQs  SSBL Lacs  ADAF FSRQs  SS L BLR /L Edd divides BL Lacs from FSRQsL BLR /L Edd divides BL Lacs from FSRQs Matter, not magnetic, dominatedMatter, not magnetic, dominated

52.  P r = radiation ~ L obs /  2 P e = relat. electrons P p = protons P B = B-field R jet power and accretion luminosity ~10 17 cm Shakura-Sunjaev disk: L d P jet = P e +P p +P B

53. What is a blazar? A jetted AGN, whose jet is relativistic (  ~10) and is “pointing at us”. A jetted AGN, whose jet is relativistic (  ~10) and is “pointing at us”. To be more quantitative: To be more quantitative:  view   For each blazar, 2  2 radio-loud AGN pointing elsewhere: FR I and FRII radio- galaxies

54. 3 months, 10  BL Lacs Flat Steep FSRQs LLLL Fossati et al. 1998; Donato et al. 2001

55. M/ M Edd GG, Maraschi, Tavecchio 2009 2 years– 4  Ackermann+ 2011

56. Molinari+ 2007

57. Isotropic Collimation corrected