Abstract
Polarimetry with LOFAR is somewhat different from polarimetry with, for example, the VLA or WSRT. At LOFAR frequencies, Faraday rotation is much stronger than at for example L band. The ionosphere in particular is a big nuisance. Moreover, the polarized response of (a group of) phased array stations is very different from the response of (a group of) parabolic dish antennas. This lecture focuses mainly on the physics of low frequency polarimetry, and how it affects observation planning, data processing, and imaging.
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The reader is encouraged to read these papers. Please note that these works did not use the same naming convention as is currently used. In fact, Stokes used A, B, C, and D, and Chandrasekhar I r, I l, U, and V , where I r and I l represent rectilinear (y) and linear (x) intensities, not right and left circular.
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What form does it have, exactly? Derive it yourself, but be careful about directions and signs!
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Brentjens, M.A. (2018). Polarization Imaging with LOFAR. In: Heald, G., McKean, J., Pizzo, R. (eds) Low Frequency Radio Astronomy and the LOFAR Observatory. Astrophysics and Space Science Library, vol 426. Springer, Cham. https://doi.org/10.1007/978-3-319-23434-2_10
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