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

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Connection between X-ray and Polarized Radio
Emission in the Large-Scale Jets of Quasars
Svetlana Jorstad
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X-ray Emission Processes in Large-Scale Jets
1. Synchrotron radiation from radio to X-ray
wavelengths (S?-a 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 0827243, 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).
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The quasar 2209080, z0.484
VLA, B-Array
VLA, A-Array
Smax0.225 Jy/beam, rms0.04 mJy/beam
Smax0.167 Jy/beam, rms0.03 mJy/beam
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Electric Vector and Faraday Rotation
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Degree of Radio Polarization and X-ray Emission
Chandra (0.2-8 keV ), ACIS-S3, 18 ks

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Chandra Observations of the Quasar 1357193,
z0.72
D. Harris et al. ACIS-S3,189ks
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VLA Observations of the Quasar 1357193
4.8 GHz
1.4 GHz
1.4 GHz
15 GHz
B-Array
A-Array
A-Array
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Radio Spectral Indices and Faraday Rotation
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Degree of Radio Polarization and X-ray Emission
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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.