1. Jets at different scales and the connection with accretion L. Maraschi and F.Tavecchio INAF - Osservatorio Astronomico di Brera

2. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Outline Can probe small and large scales within the same jetCan probe small and large scales within the same jet  The power connection within jets  The power connection within jets Can probe jet and accretion disk in the same AGNCan probe jet and accretion disk in the same AGN  The power connection between jets and accretion  The power connection between jets and accretion

3. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera To extended jet The blazar em.reg. The accretion disk

4. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Jet scales Resolved X-ray jet 10 – 100 kpc scale Blazar emission region sub-pc scale sub-pc scale Accretion region Jet origin Jet origin R_S scale R_S scale SynchroEC/CMB

5. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Radiation mechanisms Synchro+IC (on different photons)in all regions W(Radiation Energy Density)W(Radiation Energy Density) K (rel. El. Density), B (mag.F.)K (rel. El. Density), B (mag.F.) Delta/gamma (beam./Lorentz factor)Delta/gamma (beam./Lorentz factor) Essential parameters: 4Essential parameters: 4 Conditions: 4 (from the seds)Conditions: 4 (from the seds) Blazar reg: ls, lc, 2 peak frequenciesBlazar reg: ls, lc, 2 peak frequencies Large scale: ls, lc, equipart., CMBLarge scale: ls, lc, equipart., CMB

6. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Blazars: the SEDs FSRQ BL Lacs Fossati et al. 1998; Donato et al. 2001 RED BLUE ThTh thth Spectral Energy Distributions of the jet cores: Two components, synchrotron and Inverse Compton : Gamma – rays important to constrain model parameters

7. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Chandra: probing large-scale jets PKS 0637-752: the first Chandra jet Schwartz et al. 1999 Tavecchio et al. 2000; Celotti et al. 2001 Interpretation: IC from CMB

8. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Gamma-ray Blazars with resolved X-ray jets In the survey of radio jets selected to look for extended X-ray emission with CHANDRA (Sambruna et al. 2002,2004) two known gamma-ray blazars satisfied the survey criteria and extended X-ray emission was found. One gamma-ray blazar in the survey of Marshall et al 2004 Three other gamma-ray blazars were later observed with Chandra and showed extended X-ray emission. Tavecchio et al. 2005, Tavecchio et al. in preparation

9. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Subpc and kpc-scale comparison for same jet Subpc and kpc-scale comparison for same jet 1641+399 (z=0.59) 1641+399 (z=0.59) B=3G; R=4x10 16 cm; K=2.8x10 3 cm -3  =10-5 B=1.7x10 -5 G; R=2x10 22 cm; K=4x10 -6  =8-4

10. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera 1510-089 (z=0.36) 1510-089 (z=0.36) B=1.4G; R=3x10 16 cm; K=7x10 2 cm -3  =20-10 B=6x10 -6 G; R=1.3x10 22 cm; K=5x10 -6  =16-9 Subpc and kpc-scale comparison

11. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Extended jets from gamma-ray blazars 2251 1229 0954

12. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Large scale jet Small scale jet + acc. disk

13. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

16. Comparison of Lorentz factors and Powers estimated for the same jets at small (subpc) and large (100 kpc) scales Tavecchio et al. 2006 subm.

17. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera From subpc to kpc scale The bulk Lorenz factor of the jet appears consistent from subpc to 100 kpc scales but decreases close to the hot spots (some hot spots are weakly relativistic) The bulk Lorenz factor of the jet appears consistent from subpc to 100 kpc scales but decreases close to the hot spots (some hot spots are weakly relativistic) The transported power at the two scales is similar (negligible dissipation until the “end”) The transported power at the two scales is similar (negligible dissipation until the “end”) The pressure (magnetic field) at the two scales is consistent with a relation p  A -1 (B  r -1 ) The pressure (magnetic field) at the two scales is consistent with a relation p  A -1 (B  r -1 ) free expansion (high power jets)

18. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera The deep CHANDRA exposures of the cores of 1136 –135 and 1150 +497 plus an XMM observation of 0723+679 allow to disentangle the accretion disk contribution from the jet contribution in the X ray spectra which show weak Fe emission (see Grandi and Palumbo 2004 for 3C 273) We can add new data on the gamma-ray blazars and on J0754 recently discovered with SWIFT Sambruna et al. 2006 subm. Tavecchio et al 2006 in prep The Jet - Disk Connection

19. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Accretion power BZ or BP Jet power blue bump or emission lines L disk  Blazar SEDs (MT02: power estimated with parameters derived from radiative models) Energy in lobes (RS91) VLBI jets (CPG ) ThTh Connecting accretion and jet power: the concept

20. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Accretion disk: Blue Bump and X-ray p.l. Jet : Synchrotron and Inverse Compton components Blazar cores of resolved X-ray jets: disentangling disk and jet

21. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Jet Power vs. Jet Luminosity The radiative efficiency of jets in the inner (or blazar) region spans two orders of magnitude and is rather high Without protons jets would not survive the inner region

22. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Jet power vs. accretion power Maraschi & Tavecchio, 2003 Sambruna et al.2006, At high P P jet = Pacc disk At low P P jet > L disK P jet > L disK If P jet ~ P disk  < 0.01

23. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Conclusions The radiative models yield a very consistent picture of physical properties and propagation for powerful jets. The near equality of jet power and accretion power is remarkable. We derive this result for aligned jets, but in a unified scheme it should hold for all powerful radio sources. The radio-loud radio-quiet diversity still waits to be understood.

24. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

25. 1136-135 A deep exposure with Chandra HST and VLA After knot B the X-ray emission fades while the radio brightens

26. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera SEDs change from Syncro to IC-like

27. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

28. 1150+497 A deep exposure with Chandra and HST

29. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Evolution of paramaters derived from “standard” modeling of the knots SED Using the  and applying the adiabatic deceleration by Georganopoulos and Kazanas 2004 the evolutionof B and K can be computed (dashed lines)

30.  c A =       c A o + ∫  v ent dS (  w  2 c 2 +  p ) A = const w=  c 2 +4p   w  c A =   o w o   c A o + ∫  c 2 v ent dS Deceleration from entrainment Bicknell 1994

31. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Solution of the conservation equations with entrainment The amount of entrained matter necessary to explain deceleration is 10% of the transported mass

32. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera About superunification A simple scaling of the results (same external conditions same Gamma-bulk) shows that the deceleration length depends on the jet mass flux divided by the cross section radius, presumably proportional to the BH mass. Therefore the same quantity, Mdot/M determines the Sequence of Blazar SEDs, the radiative properties of the associated disks and the major morphological difference (deceleration scale) of FR I and FR II jets. We believe these are strong arguments to propose Mdot/M as a fundamental parameter in unified schemes for radiosources. We propose that the second fundamental parameter characterizing radio loudness is the black hole spin.

33. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera m Optically thin hot flow Optically thick disc j Weak or no jet Powerful jet The fundamental AGN plane FSRQ FR II FR I BL Lac

34. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Tavecchio et al. 2000 Constraints on EC/CMB and SSC models (for 0637-052)

35. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera From subpc to kpc scale ThTh

36. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Tavecchio et al. 2006 in prep

37. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Breraknots hot spots upper limits

38. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera The radio to X-ray ratio increases along the jet The radio to X-ray ratio increases along the jet

39. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Survey results Most detected knots emit X-rays via IC-CMB The synchrotron knots are those closest to the nucleus The X-ray to radio flux ratio tends to decrease along the jet See also survey of Marshall et al. 2005 In two cases large and small scale of the same jet can be compared Tavecchio et al. 2004

40. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera The blazar sequence is understood as a sequence in Powerful jets go with bright disks (high m) Powerful jets go with bright disks (high m) Optical signatures of disks in less powerful jets may be absent due to radiative inefficiency (ADAF) (low m) This is supported by direct determination of the parameters This is supported by direct determination of the parameters Maraschi 2001; Boettcher & Dermer 2002; Cavaliere & D’ Elia 2002; Maraschi & Tavecchio 2003; m

41. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Modeling the SED sequence : Ghisellini et al. 1998 Magnetic field, particle densities and radiation densities decrease along the sequence Beaming factor constant Kinetic power can be estimated and decreases along the sequence

42. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera Intensity profiles along the jet

43. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera A Chandra-HST survey of jets 17 “radio selected” jets 10 new X-ray jets (59%) 10 optical jets 9 X-ray and optical Sambruna et al. 2002 Sambruna et al. 2004 All (except 1) powerful FR II at large distances