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G. Chartas (PSU), H.L. Marshall (MIT), K.K. Ghosh (NASA/MSFC), M. Cresitello-Dittmar (SAO), W. Cui (MIT), E.D. Feigelson (PSU), D.E. Harris, E.J. Hooper (SAO), D.L. Jauncey (ATNF/CSIRO), D.-W. Kim (SAO), J. Lovell (ATNF/CSIRO), S. Mathur (OSU), D.A. Schwartz (SAO), S.J. Tingay (JPL), S.N. Virani, B.J. Wilkes (SAO), D. Worrall (SAO/Bristol)
The core-dominated radio-loud quasar PKS 0637-752 was observed with the Chandra X-ray Observatory during the orbital activation and checkout phase. The original purpose of these particular calibrations were to observe a point like source to establish an accurate focus position, and accurately determine the aim point. An early surprise in the mission was the detection of a remarkable X-ray jet. PKS 0637-752 was observed with a variety of detector configurations with a total exposure time of about 100ks. A careful spatial analysis of all the available X-ray observations reveals a jet that extends approximately 10'' to the west with a curvature very similar to the one seen in the radio observations. The X-ray intensity distribution is very similar to the radio morphology. Chandra's spatial resolving power of ~ 0.4'' allows us to spatially resolve the luminosities and spectra of the core, jet and knot. The X-ray luminosity of the core appears to have not changed since it was last observed with ASCA at \log{LX} ~ 45.8 erg/s (2-10 keV). The jet has \log{LX} ~ 44.5 erg/s. We present fits from a variety of emission models to the observed spectra, and comment on the existence of emission lines recently reported in the ASCA observations of PKS0637-752.
This work was supported by NASA grant NAS 8-38252