Fig. 26
Faraday RMs in the Galactic plane (| bII | < 5°) compared to (left to right): dust angle dispersion; dust polarization fraction at 353 GHz; synchrotron polarization fraction at 1.4 GHz; and synchrotron polarization fraction at 30 GHz. The overplotted lines show the result of a simple linear fit between the two data sets, with the Pearson correlation coefficient r quantifying the degree of correlation. The colour scale shows the pixel density on a log10 scale.
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