We present Chandra X-ray ( 0.2-8 keV ) and Very Large Array radio ( 15 and 5 GHz ) images of the \gamma -ray bright , superluminal quasar 0827+243 .
The X-ray jet bends sharply—by \sim 90 ^ { \circ } , presumably amplified by projection effects—5 ^ { \prime \prime } 
from the core .
Only extremely weak radio emission is detected between the nuclear region and the bend .
The X-ray continuum spectrum of the combined emission of the knots is rather flat , with a slope of -0.4 \pm 0.2 , while the 5-15 GHz spectra are steeper for knots detected in the radio .
These characteristics , as well as non-detection of the jet in the optical band by the Hubble Space Telescope , pose challenges to models for the spectral energy distributions ( SEDs ) of the jet features .
The SEDs could arise from pure synchrotron emission from either a single or dual population of relativistic electrons only if the minimum electron energy per unit mass \gamma _ { min } \gtrsim 1000 .
In the case of a single population , the radiative energy losses of the X-ray emitting electrons must be suppressed owing to inverse Compton scattering in the Klein-Nishina regime , as proposed by Dermer & Atoyan .
Alternatively , the X-ray emission could result from inverse Compton scattering of the Cosmic Microwave Background photons by electrons with Lorentz factors as low as \gamma \sim 15 .
In all models , the bulk Lorentz factor of the jet flow \Gamma \gtrsim 20 found on parsec scales must continue without substantial deceleration out to 800 kpc ( deprojected ) from the nucleus , and the magnetic field is very low , \lesssim 2 \mu G , until the bend .
Deceleration does appear to occur at and beyond the sharp bend , such that the flow could be only mildly relativistic at the end of the jet .
Significant intensification of the magnetic field occurs downstream of the bend , where there is an offset between the projected positions of the X-ray and radio features .