Svetlana Jorstad

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

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

The quasar 2209+080, z=0.484

Smax=0.225 Jy/beam, rms=0.04 mJy/beam

Smax=0.167 Jy/beam, rms=0.03 mJy/beam

VLA, B-Array VLA, A-Array

Electric Vector and Faraday Rotation

Degree of Radio Polarization and X-ray Emission

Chandra (0.2-8 keV ), ACIS-S3, 18 ks

Chandra Observations of the Quasar 1357+193, z=0.72

D. Harris et al.

ACIS-S3,189ks

1.4 GHz

A-Array

4.8 GHz

1.4 GHz

VLA Observations of the Quasar 1357+193

15 GHz1.4 GHz

A-Array B-Array

Radio Spectral Indices and Faraday Rotation

Degree of Radio Polarization and X-ray Emission

Conclusion

Polarization observations of large-scale radio jets of quasars alongwith 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.