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Galaxies 2018, 6(4), 140; https://doi.org/10.3390/galaxies6040140

Faraday Tomography Tutorial

1
Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, NL-6500 GL Nijmegen, The Netherlands
2
Graduate School of Science and Technology, Kumamoto University, 2-39-1, Kurokami, Kumamoto 860-8555, Japan
3
CSIRO Astronomy and Space Science, P.O. Box 1130, Bentley, WA 6102, Australia
*
Author to whom correspondence should be addressed.
Received: 16 November 2018 / Revised: 6 December 2018 / Accepted: 12 December 2018 / Published: 14 December 2018
(This article belongs to the Special Issue The Power of Faraday Tomography)
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Abstract

The capabilities of wide-band polarization datasets that are now becoming available from precursors/pathfinders to the Square Kilometre Array (SKA), and eventually from the SKA itself, make it possible to use the Faraday tomography technique to facilitate the study of cosmic magnetism. While many programs enabling Faraday tomography have been developed by various authors and it is now becoming easier to apply the required techniques, the interpretation of the results is not straightforward. This is not only because of the lack of a one-to-one relation between the Faraday depth and the physical depth, and observational artifacts such as instrumental polarization, but also because the choice of the method that is used and its settings can be reflected in the results. Thus, it is essential to understand how the various methods enabling Faraday tomography are suited for the efficient application of the technique. In the workshop “The Power of Faraday Tomography”, we organized a Faraday tomography tutorial to help the participants understand the required tools. In this article, we summarize the basics of the techniques, and provide an overview of the tutorial. View Full-Text
Keywords: magnetic fields; polarization; techniques: polarimetric magnetic fields; polarization; techniques: polarimetric
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Ideguchi, S.; Miyashita, Y.; Heald, G. Faraday Tomography Tutorial. Galaxies 2018, 6, 140.

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