1. Modeling and Understanding of Blazar Sources Gabriele Ghisellini INAF – Osservatorio Astronomico di Brera G. Bonnoli, A. Celotti, L. Foschini, G. Ghirlanda, L. Maraschi, F. Tavecchio With the help of: G. Bonnoli, A. Celotti, L. Foschini, G. Ghirlanda, L. Maraschi, F. Tavecchio

2. Fermi blazars

3. 3 months, 10 

7. Fossati et al. 1998; Donato et al. 2001

8. F  =k F r P~10 -17 0.8 Ghirlanda+ 2010 20 GHz southern sources with F>40mJy: 3600 radio flat sources, 230 associations with Fermi blazars

9. F  =k F r 0.8 Only 1/15 of the radio sources are detected by LAT Ghirlanda+ 2011

10. F  =k F r Ghirlanda+ 2011 1 2 3: number Assume a slope and a dispersion (  -variability)

11. 3 months, 10  BL Lacs Flat Steep FSRQs LLLL Fossati et al. 1998; Donato et al. 2001

12. 11 months – 4  Abdo+ 2010 BL Lacs FSRQs

13. 11 months – 4  Abdo+ 2010 Intruder BL Lacs?

14. 0208- 512 11 months – 4  Scarpa & Falomo 1997 L MgII =1.75x10 44 erg/s EW=5A

15. When a BL Lac is a BL Lac?  Usually, EW< 5A  Easy, but not physical  Better to measure L BLR  But normalize it to L Edd

16. ~5x10 -4 GG+ 2011

17. Sbarrato+ in prep SDSS+1LAC Do we really need to divide blazars?

18. TeV blazars

19. 107 sources: 46 extragal + 61 gal http://www.mpp.mpg.de/~rwagner/sources/

21. Also FSRQs ! http://www.mpp.mpg.de/~rwagner/sources/

22. Also Radio-galaxies ! http://www.mpp.mpg.de/~rwagner/sources/

23. Also starbursts galaxies! http://www.mpp.mpg.de/~rwagner/sources/

24. Crab level ~15 Crab Aharonian et al. 2007 t var ~ 3-5 min !<< R S /c PKS 2155-304

25. 10 4 t var ~ 10 4 M 9 seconds (3 h) 1/  RSRS d ~ 10 2 -10 3 R S ~  2 R S R~d/  t var ~d/  2  R s R s R s d=~   R S RsRs Internal shocks Blob

26. 

27.  

28.  Jet in a jet

29.  Needle (rifle)

30. GG+2009: needle Giannios +2009: jet in a jet by reconnection

31. GG+2009 Giannios +2009 For 2155-304: No strong disk, no severe cooling, e- can reach high energies

32. Aleksic+ 2011 – MAGIC 1222+216 z=0.432: a FSRQ! 10 min

33. Tavecchio+ 2011

34. GG+2009 Giannios +2009 For 1222+216: Strong disk, severe cooling, e- cannot reach high energies. Plenty of external seeds, no need to be inside the “normal” emitting region

35. GG+2009 Giannios +2009

36. Cosmic B-background

37. TeV no GeV Tavecchio+ 2010

38. blazar

39. LHC Reprocessed GeV  intergalactic B Reprocessed GeV  intergalactic B

40. ~10 TeV ~10 GeV   ~1 with IR bkg IC with CMB With no B-field A simplified view: see Neronov+ 2010; Tavecchio+ 2010 e+e-

41. ~10 TeV ~10 GeV   ~1 with IR bkg IC with CMB With no B-field Neronov+ 2010 – Tavecchio+ 2010

42. With B-field Neronov+ 2010 – Tavecchio+ 2010

43. Big blazars

44. 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

45. Torus ~1-10 pc Broad Line Region ~0.2 pc ~VLBI region ~20 pc away (Marscher+)  R BLR R Torus disk Lyutikov

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

47. Blazars also present in SDSS (DR7) FWHM + estimate of R BLR

48.  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

49. P r ~ L obs /  2 ”model independent” P r is the absolute minimum of P jet P r =L d

50. P r ~ L d P r ~ Mc 2 L d ~ M 2 c 2 P r ~ L d 1/2

51. If one proton per emitting electron P j =L d

52. 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

53. When a massive and dormant BH wakes up

54. Burrows+ astro-ph/1104.4787 Swift/XRT 110328A = Swift 1644+57

55. Levan+ astro-ph/1104.3356 (30 mas) HST: < 150 pc from center (30 mas) VLBI: < 2.5 pc (0.5 mas, Atel 3269)

56. Levan+ astro-ph/1104.3356 A small starburst galaxy Total mass = 10 9 -10 10 M O M BH ~ 10 6 -10 7 M O z=0.3534

57. Burrows+ astro-ph/1104.4787 TNG

58. Burrows+ astro-ph/1104.4787 t -5/3 Swift/XRT 110328A = Swift 1644+57 Tidal disruption of a star + formation of a relativistic jet

59. TNG XRT Burrows+ astro-ph/1104/4787

60. Burrows+ astro-ph/1104.4787 F( ) ~ 1/3 A V =4.5

61. Burrows+ astro-ph/1104.4787 Particle-starved  Poynting dominated P B ~10 46 erg/s Reconnection?

62. L=0.01 L Edd

63. 1644+57? Late prompt in GRBs?

64. Conclusions Find why radio-quiet/radio-loud Find if it is BZ Find if jets are more efficient than accretion Marek, you now start your second half of your carrier: you cannot rest!