Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637–752

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Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637–752

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Title: Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637–752
Author: Schwartz, D. A.; Marshall, H. L.; Lovell, J. E. J.; Piner, B. G.; Tingay, S. J.; Birkinshaw, M.; Chartas, G.; Elvis, Martin S.; Feigelson, E. D.; Ghosh, K. K.; Harris, D. E.; Hirabayashi, H.; Hooper, E. J.; Jauncey, D. L.; Lanzetta, K. M.; Mathur, S.; Preston, R. A.; Tucker, W. H.; Virani, S.; Wilkes, Belinda Jane; Worrall, Diana M.

Note: Order does not necessarily reflect citation order of authors.

Citation: Schwartz, D. A., H. L. Marshall, J. E. J. Lovell, B. G. Piner, S. J. Tingay, M. Birkinshaw, G. Chartas, et al. 2000. “Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637–752.” The Astrophysical Journal 540 (2) (September 10): L69–L72. doi:10.1086/312875.
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Abstract: The quasar PKS 0637-752, the first celestial X-ray target of the Chandra X-Ray Observatory, has revealed asymmetric X-ray structure extending from 3'' to 12'' west of the quasar, coincident with the inner portion of the jet previously detected in a 4.8 GHz radio image (Tingay et al. 1998). At a redshift of z = 0.651, the jet is the largest (gsim100 kpc in the plane of the sky) and most luminous (~1044.6 ergs s-1) of the few so far detected in X-rays. This Letter presents a high-resolution X-ray image of the jet, from 42 ks of data when PKS 0637-752 was on-axis and ACIS-S was near the optimum focus. For the inner portion of the radio jet, the X-ray morphology closely matches that of new Australian Telescope Compact Array radio images at 4.8 and 8.6 GHz. Observations of the parsec-scale core using the very long baseline interferometry space observatory program mission show structure aligned with the X-ray jet, placing important constraints on the X-ray source models. Hubble Space Telescope images show that there are three small knots coincident with the peak radio and X-ray emission. Two of these are resolved, which we use to estimate the sizes of the X-ray and radio knots. The outer portion of the radio jet and a radio component to the east show no X-ray emission to a limit of about 100 times lower flux. The X-ray emission is difficult to explain with models that successfully account for extranuclear X-ray/radio structures in other active galaxies. We think the most plausible is a synchrotron self-Compton model, but this would imply extreme departures from the conventional minimum energy and/or homogeneity assumptions. We also rule out synchrotron or thermal bremsstrahlung models for the jet X-rays, unless multicomponent or ad hoc geometries are invoked.
Published Version: doi:10.1086/312875
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