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

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

  2. X-ray Emission Processes in Large-Scale Jets 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).

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

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