The Structure and Physics of Extragalactic Jets

Details The Structure and Physics of Extragalactic Jets The Structure and Physics of Extragalactic Jets

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9142p&link_type=abstract

HST Proposal ID #9142

Physics

Hst Proposal Id #9142 Agn/Quasars

Scientific paper

As part of an ongoing investigation into the physics of jets, we propose to obtain WFPC2 polarimetry of the jets of 3C 264 and 3C 78. We are motivated by our recent findings of strong radio-optical polarimetry differences in the M87 jet, which imply that radio and optical synchrotron emitting electrons must occupy physically distinct regions, with high- energy particles concentrated closer to the jet axis, and affected more by shocks, than lower-energy particles. This is the first clear evidence regarding the internal structure of a relativistic jet. Here we propose to test whether our model holds in jets with different morphologies and luminosities, by obtaining high-resolution optical polarimetry of a sample of optical jets. This will produce fundamental gains in our knowledge of the structure and physics of extragalactic jets. By comparing the total intensity and polarized structures in the optical and radio, we will probe the magnetic field configurations in both optical and radio emitting regions. This will allow us to test the level of stratification in these jets, and uncover whether the magnetic field geometry is largely fixed at formation, or dominated by subsequent flow dynamics. By adding to the picture our optical spectral information, we will gauge the impact of shocks, the need for in situ particle acceleration, and test jet models.

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