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D. A. Schwartz (CfA), H.L. Marshall (MIT), J.E.J. Lovell, S.J. Tingay, D.L. Jauncey (ATNF/CSIRO), B.G. Piner, R.A. Preston (JPL), M. Birkinshaw, D.M. Worrall (U. Bristol), G. Chartas, E.D. Feigelson (Penn State), M. Elvis, E.J. Hooper, W.H. Tucker, S. Virani (CfA), K.K. Ghosh (MSFC), H. Hirabayashi (ISAS), K.M. Lanzetta (SUNY/Stony Brook), S. Mathur (OSU)
We use the CXC CIAO software to fit models of the spatial structure of the X-ray jet emitted from the quasar PKS0637-752. After careful assessment of scattering from the central source, and establishing a limit to any X-ray emission from the cluster, we detect X-ray emission from the eastern radio knot and past the bend of the radio jet to the northwest. We attempt to fit the bright western jet as either a series of point sources only, or as points at the 4 brightest knots with a spatially continous cylinder from 4 to 11 arcsec west of the nucleus. The fits lead to a wide range of intrinsic parameters, depending on whether the jet is non-relativistic and in the plane of the sky, or is relativistic and pointing within 6 degrees of our line of sight as shown by VLBI monitoring for the pc scale jet in the quasar nucleus.
This research has been sponsored by the ISAS/VSOP project, CSIRO, and several NASA contracts and grants including NAS8-39073 to the Chandra X-ray Center.
The author(s) of this abstract have provided an email address for comments about the abstract: das@cfa.harvard.edu