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D.A. Schwartz (Harvard-Smithsonian CfA), H.L. Marshall (MIT), J. Drake, A. Fruscione, J. Grimes, D. Harris, R. Kraft, S.S. Murray, D. Pease, A. Siemiginowska, S. Vrtilek (Harvard-Smithsonian CfA)
We have used the CXC CIAO software to fit spatial models to an ACIS-S observation of the X-ray jet in 3C 273. We have a total of 3943 counts, 0.5 to 8 keV, from the bright portion of the jet, 10 to 22 arcsec from the quasar core. Our best fits resolve the bright radio knots. To fit the entire X-ray emission with localized circular Gaussians requires more than 11 knots; therefore, we investigate a model with a continuous X-ray jet plus localized knots. We use the intensities fit to these knots to re-examine their SED from radio through X-rays, and assess the X-ray emission mechanism. We will report on investigation of energy dependence of the X-ray morphology.
This research has been sponsored by 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