1. C.C. Teddy Cheung NASA Goddard Space Flight Center and Eureka Scientific Inc.* Teddy.Cheung@nasa.gov Radio Galaxies in the Chandra Era 8 July 2008 *Chandra GO7-8114C High Redshift Relativistic Jets

2. The Near, the Anticipated Chandra View of Cen A J. Goodger R. Kraft C. Jones (earlier) Kraft et al. (2001) 3C273 ROSAT H. Marshall Roser et al. (2000) M87 Einstein, VLA grayscale Biretta et al. (1991) D. Harris (earlier)

3. Nearby (z<0.1) low-power FRIs Continuous steep declining spectra X-ray variability Canonical synchrotron behavior Sites of particle acceleration The Near, the Anticipated SEDs compiled by Brunetti (2001) 3C66b (Hardcastle et al. 2001); B2 0755 (Worrall et al. 2001)

4. Superluminal ( β app ~10c) quasar PKS 0637-752 (z=0.65) Very large jet: ~100/sin θ kpc = 600 kpc ( θ =10 o ) The Far, the Unanticipated Chartas et al. (2000) Schwartz et al. (2000)

5. High-z Jets: a Different Phenomenon PKS 0637 knot SED SED from Uchiyama et al. (2006) See Chartas et al., Schwartz et al. (2000) Tavecchio et al. (2000) and Celotti et al. (2001)

6. High-z Jets: a Different Phenomenon PKS 0637 knot SED Recall the FRIs looked like… SED from Uchiyama et al. (2006) See Chartas et al., Schwartz et al. (2000) Tavecchio et al. (2000) and Celotti et al. (2001) Trough Peaked

7. Inverse Compton scattering of CMB? SED from Uchiyama et al. (2006) See Chartas et al., Schwartz et al. (2000) Tavecchio et al. (2000) and Celotti et al. (2001) PKS 0637 knot SED U CMB  α  (1+z) 4 = 7.5x larger at z=0.65 Requires Γ 2 boosting ( Γ ~3-15 on 100’s kpc) Requires Υ min ~10’s-100, implying large jet powers, 10 48 ergs/s Jets inferred to be near equipartition (U B ~U part. )

8. The Far and Very Far

9. Separate phenomena at low-z ( 0.1) ‘Excess’ X-rays symptom of z>0.1 jets (except Pic A – Wilson et al. 2001, Hardcastle & Croston 2005; 3C353 – Kataoka et al. 2008)

10. Separate phenomena at low-z ( 0.1) ‘Excess’ X-rays symptom of z>0.1 jets (except Pic A – Wilson et al. 2001, Hardcastle & Croston 2005; 3C353 – Kataoka et al. 2008) Ubiquitous problem (32 of 88 sources listed in XJET) The Far and Very Far This talk

11. Synchrotron vs. Inverse Compton See Felten & Morrison 1966, Blumenthal & Gould 1970, Harris & Grindlay 1979, Schwartz 2002 υ X F X  υ R F R α  (1+z) 0 [synchrotron, ‘conventional’ models] υ X F X  υ R F R α  (1+z) 4 Γ 2 [IC/CMB]

12. υ X F X  υ R F R α  (1+z) 0 [synchrotron, ‘conventional’ models] υ X F X  υ R F R α  (1+z) 4 Γ 2 [IC/CMB] Synchrotron vs. Inverse Compton See Felten & Morrison 1966, Blumenthal & Gould 1970, Harris & Grindlay 1979, Schwartz 2002 We expect many bright X-ray jets at high- redshift even with modest beaming… So where are they?!?

13. Very high-z Jet? Schwartz (2004); ROSAT X-ray color and Radio Contours GB J1713+2148, z=4 quasar Apparent ‘jet knot’ in NVSS map (45” resolution) coincident with bright ROSAT source

14. Very high-z Jet? Schwartz (2004) GB J1713+2148, z=4 quasar Apparent ‘jet knot’ in NVSS map (45” resolution) coincident with bright ROSAT source z=4 quasar no radio jet Field source with radio jet Arcsec-resolution radio maps necessary for such studies

15. X-ray Jet in Radio Quiet AGN? Schwartz et al. (2004) Optical grayscale; X-ray contours Extended X-ray feature but quasar is radio-quiet: F(4cm) <0.2 mJy No radio jet: low Υ max ? If IC/CMB X-ray jet, lack of optical emission implies very narrow particle distribution: Υ min ~10’s, Υ max ~1000’s Current studies ‘biased’ toward radio-selected jets: need possible deeper radio (EVLA) Jet? Quasar CXOMP J0841+131 z=1.9

16. X-ray Jet in Radio Quiet AGN? Schwartz et al. (2004) Optical grayscale; X-ray contours Jet? Remember Pictor A! X-ray bright, radio faint jet Extended X-ray feature but quasar is radio-quiet: F(4cm) <0.2 mJy No radio jet: low Υ max ? If IC/CMB X-ray jet, lack of optical emission implies very narrow particle distribution: Υ min ~10’s, Υ max ~1000’s Current studies ‘biased’ toward radio-selected jets: need possible deeper radio (EVLA) Wilson et al. (2001) Quasar CXOMP J0841+131 z=1.9

17. Another X-ray (only) Jet at z=4.3? Over 100 counts in 2.5” knot (17 kpc projected) in 90 ksec exposure Siemiginowska et al. (2003) See also Yuan et al. (2003)

18. Known variable X-ray and flat- spectrum radio source (blazar) U CMB  α  (1+z) 4 = 100x larger than PKS 0637 (z=0.65) No previously known radio jet… Another X-ray (only) Jet at z=4.3? Over 100 counts in 2.5” knot (17 kpc projected) in 90 ksec exposure Siemiginowska et al. (2003) See also Yuan et al. (2003)

19. Radio/X-ray Jet at z=4.3 Here it is! Siemiginowska et al. (2003) See also Yuan et al. (2003) Cheung (2004) Radio contours, Chandra color

20. Radio/X-ray Jet at z=4.3 Cheung, Chatterjee, Brisken VLBA pc-scale jet Large projected bend in jet Cheung (2004) Radio contours, Chandra color

21. Radio/X-ray Jet at z=4.3 Cheung (2004) Radio contours, Chandra color

22. Radio/X-ray Jet at z=4.3 Cheung (2004) Radio contours, Chandra color υ r F r υ x F x

23. Redshift Dependence? Cheung (2004) υ x F x υ r F r --------

24. Redshift Dependence? Cheung (2004) (setting alpha=1) See Tavecchio et al. (2006) = -------- υ x F x υ r F r

25. Powerful jet (L R =4x10 44 erg/s; L X ~10 L R ) Resolved jet structure (rather than single feature) B=… T_electron T_lightcross Another High-z Jet, at z=3.9 Cheung, Stawarz, Siemiginowska (2006); only 20 ksec Chandra exposure X-ray color and contours Radio color, X-ray contours

26. And Several More… J2219-2719 Chandra detection Lopez et al. (2006) Chandra cycle 7 snapshots of radio jets (with Stawarz, Siemiginowska, Schwartz, Harris, Wardle, Gobeille, Lee) Detections (top row) non-detections (bottom row)

27. High-z Jet SEDs υ x F x υ r F r Additional 5 GHz detection of GB1508 knot (Cheung, Wardle, Lee 2005)

28. Redshift Dependence?

29. Redshift (and Beaming) Dependence? Lobe-dominated radio quasars Includes several new (Cheung, Marshall, Hough, Bridle, Wardle)

30. Redshift (and Beaming) Dependence? Larger δ increases fx/fr Lobe-dominated radio quasars Includes several new (Cheung, Marshall, Hough, Bridle, Wardle)

31. Four Challenges X-ray emission mechanism and physics through high-redshift jets [Radio imaging needs to catch up]

32. Jet Deceleration at High-redshift? Kataoka & Stawarz (2005) At high-z, increase IGM density and clumpiness Increased dissipation; jets stifled - more disrupted (pc & kpc) morphologies? Slower jets? More rapid deceleration to kpc-scales?

33. Triples to Same Linear Scale z = 3.891z = 3.818z = 3.464z = 3.244z = 3.076 z = 3.035z = 2.877z = 2.732z = 2.707z = 2.686 z = 2.660z = 2.647z = 2.582 342 kpc x 342 kpc boxes Radio Imaging: Catching Up SDSS/FIRST quasars; 154 sources z=2.5 – 5.5 Wardle, Gobeille, Cheung poster

34. Four Challenges X-ray emission mechanism and physics through high-redshift jets [Radio imaging needs to catch up] Synergy with gamma-ray (GLAST) observations [Chandra imaging of GLAST-LAT blazars]

35. Large-scale Jets as g-ray Sources From Georganopoulos et al. (2006) See Marshall et al. (2001), Sambruna et al. (2001), Uchiyama et al. (2006), Jester et al. (2006) 3C273

36. Energy Transport from sub-pc / kpc Tavecchio et al. (2005, 2007); also Schwartz et al. (2006) See talks by Jorstad, Marscher Poster by Hogan (MOJAVE sources)

37. Leaving no g-ray Blazar Behind See: http://glast.gsfc.nasa.gov/ssc/data/policy/LAT_Monitored_Sources.html VLBA 2cm Survey map of PKS 1622-297 Extended 14” feature – no map (Perley 1982) Antonucci et al. (1986) Reid et al. (1999) NRAO 530 – 1 min. snapshot S5 0716+714

38. Four Challenges X-ray emission mechanism and physics through high-redshift jets [Radio imaging needs to catch up] Synergy with gamma-ray (GLAST) observations [Chandra imaging of GLAST-LAT blazars] The low-energy spectra [Anticipate Chandra data necessary when LWA, LOFAR come online]

39. Where are the Low-E electrons? In my opinion, if the LWA does nothing more than tell us something new about the low end of relativistic electron spectra, it would have been worth the effort! -D.E. Harris (2005), Clark Lake to Long Wavelength Array Meeting

40. Where are the Low-E electrons? PKS 0637-752 knot SED Inferred low-freq spectrum Tavecchio et al. (2000) Schwartz et al. (2000); Chartas et al. (2000) Harris & Krawczynski (2006)

41. The Case of 3C273 Originate from the same relativistic electrons… What about lower- frequency emission?

42. The Case of 3C273 Originate from the same relativistic electrons… MERLIN 151 MHz Conway et al. (1993)

43. The Case of 3C273 Originate from the same relativistic electrons… MERLIN 151 MHz Conway et al. (1993)

44. The Case of 3C273 Originate from the same relativistic electrons… MERLIN 151 MHz Conway et al. (1993) Marshall et al. (2001) – Herman’s talk

45. The Case of 3C273 MERLIN 151 MHz Conway et al. (1993) Jet Core

46. The Case of 3C273 MERLIN 151 MHz Conway et al. (1993) Jet Core Spectrum extends down to 10 MHz Helmboldt et al. (2008) 4 3 2 1 Log F v (Jy) 0

47. Steep-spectrum Excess Sources How many others are there? Cheung, Stawarz, Siemiginowska (2006)

48. Low-frequency Spectral Curvature

49. Low-frequency break reduces L R ; L X unchanged Could explain flatter X-ray spectra ( α  X < α R ) May reduce the very large inferred δ factors Possible explanation for discrepant B-field estimates in radio clusters/relics (Petrosian 2001)

50. Four Challenges X-ray emission mechanism and physics through high-redshift jets [Radio imaging needs to catch up] Synergy with gamma-ray (GLAST) observations [Chandra imaging of GLAST-LAT blazars] The low-energy spectra [Anticipate Chandra data necessary when LWA, LOFAR come online] Hybrid synchrotron + IC models? [Detailed modeling of 3C273, PKS0637-752]

51. Combined IC/CMB + Synchrotron? Dermer & Atoyan (2002) Klein-Nishina regime γ~10 8 / Γ (1+z) Flattening υ~10 17 δ B μG / Γ 2 (1+z) 3 Hz Uchiyama et al. (2006)

52. Thanks! Especially to Aneta, Ralph, the LOC, SOC & CXC