The core-dominated radio-loud quasar PKS 0637-752 ( z = 0.654 ) was the first celestial object observed with the Chandra X-ray Observatory , offering the early surprise of the detection of a remarkable X-ray jet .
Several observations with a variety of detector configurations contribute to a total exposure time with the Chandra Advanced CCD Imaging Spectrometer ( ACIS ; Garmire et al .
2000 , in preparation ) of about 100 ks .
A spatial analysis of all the available X-ray data , making use of Chandra ’ s spatial resolving power of about 0.4 arcsec , reveals a jet that extends about 10 arcsec to the west of the nucleus .
At least four X-ray knots are resolved along the jet , which contains about 5 % of the overall X-ray luminosity of the source .
Previous observations of PKS 0637-752 in the radio band ( Tingay et al .
1998 ) had identified a kpc-scale radio jet extending to the West of the quasar .
The X-ray and radio jets are similar in shape , intensity distribution , and angular structure out to about 9 arcsec , after which the X-ray brightness decreases more rapidly and the radio jet turns abruptly to the north .
The X-ray luminosity of the total source is \log L _ { X } \approx 45.8 erg s ^ { -1 } ( 2 - 10 keV ) , We use H _ { 0 } = 50 km s ^ { -1 } Mpc ^ { -1 } and q _ { 0 } = 0 throughout and appears not to have changed since it was observed with ASCA in November 1996 .
We present the results of fitting a variety of emission models to the observed spectral distribution , comment on the non-existence of emission lines recently reported in the ASCA observations of PKS 0637-752 , and briefly discuss plausible X-ray emission mechanisms .