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J ets at differe nt scales and the connection with accretion

J ets at differe nt scales and the connection with accretion. L. Maraschi and F.Tavecchio INAF - Osservatorio Astronomico di Brera. Outline. Can probe small and large scales within the same jet  The power connection within jets Can probe jet and accretion disk in the same AGN

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J ets at differe nt scales and the connection with accretion

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

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

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

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

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

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

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

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

  9. Subpc and kpc-scale comparison for same jet 1641+399 (z=0.59) B=3G; R=4x1016cm; K=2.8x103cm-3 G=10-5 B=1.7x10-5G; R=2x1022cm; K=4x10-6 G=8-4 Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

  10. Subpc and kpc-scale comparison 1510-089 (z=0.36) B=1.4G; R=3x1016cm; K=7x102cm-3 G=20-10 B=6x10-6G; R=1.3x1022cm; K=5x10-6 G=16-9 Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

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

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

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

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

  17. 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 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 pµA-1 (B µ r-1) free expansion (high power jets) Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

  18. The Jet - DiskConnection 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 Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

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

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

  22. Jet power vs. accretion power At high P Pjet = Paccdisk At low P Pjet > LdisK If Pjet ~ Pdisk e < 0.01 Maraschi & Tavecchio, 2003 Sambruna et al.2006, Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

  23. Conclusions The radiative modelsyield 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. Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

  25. 1136-135 A deep exposure with ChandraHST and VLA After knot B the X-ray emission fades while the radio brightens Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

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

  28. 1150+497 A deep exposure with Chandra and HST Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

  30. Deceleration from entrainment G r b c A = Go ro bo c Ao + ∫rvent dS (Gwb2 c2 + Dp)A = const w=r c2 +4p G2wb c A = G2owobo c Ao + ∫ r c2 vent dS Bicknell 1994

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

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

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

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

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

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

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

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

  39. Survey results Mostdetected 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 Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

  40. The blazar sequence is understood as a sequence in • 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 Maraschi 2001; Boettcher & Dermer 2002; Cavaliere & D’ Elia 2002; Maraschi & Tavecchio 2003; • • Xi’an 16-21 October 2006 Laura Maraschi INAF – Osservatorio Astronomico di Brera

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

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

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

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