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The Long, Bright Extended X-ray Jet of OJ287

The Long, Bright Extended X-ray Jet of OJ287. Alan Marscher & Svetlana Jorstad Boston University Research Web Page: www.bu.edu/blazars. Chandra Image of OJ287 (50 ks exposure). Comparison of X-ray (Chandra) and Radio (VLA) Jet.

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The Long, Bright Extended X-ray Jet of OJ287

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  1. The Long, Bright Extended X-ray Jet of OJ287 Alan Marscher & Svetlana Jorstad Boston University Research Web Page:www.bu.edu/blazars

  2. Chandra Image of OJ287 (50 ks exposure)

  3. Comparison of X-ray (Chandra) and Radio (VLA) Jet X-ray emission follows radio but extends beyond lowest VLA contour Readout streak 1 = 4.52 kpc Length of X-ray jet ~ 81 kpc in projection (before confusion with readout streak) Color: 0.2-6 keV Contours: 1.4 GHz

  4. Compact (VLBA) vs. Extended Jet VLBA • Kpc-scale jet consistent with continuation of pc-scale jet • pc scales: superluminal motion as high as 18c (Jorstad et al. 2005) • = 16.5±4.0, viewing angle = 3.2º±0.9º,  = 19±6 • Deprojected length of X-ray jet = 1.5±0.5 Mpc Radio/X-ray spectral index ~ 0.7 (we will have opt/ & IR fluxes)

  5. Luminosity of OJ287 Jet OJ287: length of X-ray jet > 1 Mpc L < 2x1024 watts/Hz at 1.4 GHz for region at end of jet (upper limit: no beaming)* • Upper range of FR 1 luminosity Extended (apparent) X-ray luminosity: 3x1042 erg/s * If there is a slower spine that decelerates with distance in OJ287, its 1.4 GHz luminosity is less than ~ 1024 watts/Hz

  6. Comparison with Extended Jets of other BL Lac Objects 2007+777 (z=0.342) (Sambruna et al. 2008) - similar, but not as high  PKS 0521-365 (z=0.0554) (Birkinshaw et al. 2002) - short jet 3C 371 (z=0.051) & PKS 2201+041 (z=0.027) (Sambruna et al. 2007) - few arcsecs long, resolved transverse to axis: Contours: radio (VLA) Color: X-ray (Chandra) 2201+041 3C 371

  7. Long, Fast FR 1 Jets Long (> 1 Mpc) jets with high : high- tail of population Rare in more local FR 1 radio galaxies Higher  jets have smaller opening angles (Jorstad et al. 2005) High  low entrainment, greater penetration into IGM without deceleration ***independent of whether FR 1 or FR 2 luminosity***

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