Svetlana Jorstad Connection between X-ray and Polarized Radio Emission in the Large-Scale Jets of Quasars.
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Presentation on theme: "Svetlana Jorstad Connection between X-ray and Polarized Radio Emission in the Large-Scale Jets of Quasars."— Presentation transcript:
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 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
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.