1. Svetlana Jorstad Connection between X-ray and Polarized Radio Emission in the Large-Scale Jets of Quasars

2. 1. Synchrotron radiation from radio to X-ray wavelengths (S ~ ν -α : 3C 273, Uchiyama et al. 2006 ). 2. Synchrotron emission from a second, much more energetic population of electrons (spine-sheath model: 1127-145, Siemiginowska et al. 2008; 0827+243, Jorstad & Marscher 2004). 3. Inverse Compton scattering off photons external to the jet (CMB provides the seed photons; Sambruna et al. 2004; Marshall et al. 2005). 4. Inverse Compton scattering off radio-to-optical synchrotron photons (SSC emission). X-ray Emission Processes in Large-Scale Jets

3. The quasar 2209+080, z=0.484 S max =0.225 Jy/beam, rms=0.04 mJy/beam S max =0.167 Jy/beam, rms=0.03 mJy/beam VLA, B-Array VLA, A-Array

4. Electric Vector and Faraday Rotation

5. Degree of Radio Polarization and X-ray Emission Chandra (0.2-8 keV ), ACIS-S3, 18 ks

6. Chandra Observations of the Quasar 1357+193, z=0.72 D. Harris et al. ACIS-S3,189ks

7. 1.4 GHz A-Array 4.8 GHz 1.4 GHz VLA Observations of the Quasar 1357+193 15 GHz 1.4 GHz A-Array B-Array

8. Radio Spectral Indices and Faraday Rotation

9. Degree of Radio Polarization and X-ray Emission

10. Conclusion Polarization observations of large-scale radio jets of quasars along with high resolution X-ray observations suggest an anticorrelation between the peaks of the X-ray emission and degree of polarization. This can be interpreted as an indication that turbulent particle acceleration is responsible for the energy gain of the relativistic electrons.