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D.A. Schwartz (Harvard-Smithsonian CfA)
We have searched for X-ray jets in the quasar PKS 2215+020. We anticipate such jets on kpc scales at large redshift due to the enhancement of the CMB energy density by the factor (1+z)4, (Schwartz 2002, ApJ(Lett), 569, L23). In this particular object, Lobanov et al. (2001, ApJ, 547, 714) have noted a slight, although not statistically significant, offset of both the ROSAT position and HRI contours in the direction of a 7'' VLA structure. Our \emph{Chandra} ACIS-S 27 ksec observation shows no sign of X-ray extension on 3 to 10 arcsec scales, with an upper limit of 0.34 nJy. We detect the quasar core with a flux density of 19 nJy at 1 keV. By comparing to the synchrotron self-Compton (SSC) emission expected from the VLBI structures observed by Lobanov et al., we can deduce a relativistic beaming factor \delta = 1/(\Gamma(1-\beta \cos \theta))=1.5. We expect that this SSC emission is responsible for the extreme value of \alphaox=0.9 reported by Seibert and Brinkmann (1998, AA, 333, 63). The pc scale jet may be at a relatively large angle to our line of sight (as suggested in Lobanov) and/or bending away from our line of sight so that we do not see beamed X-ray emission from the jet.
This work was supported by NASA contract NAS8-39073 to the \emph{Chandra} X-ray Center.
The author(s) of this abstract have provided an email address for comments about the abstract: das@cfa.harvard.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.