Extended Data Fig. 3: Variation of the Stokes Q and U parameters with magnetic field orientation.
From: Polarized thermal emission from dust in a galaxy at redshift 2.6
The B field orientation (white lines) at 5 degrees (a), 10 degrees (b), 45 degrees (c), 90 degrees (d) are shown over the Stokes I (a), Stokes Q (e), Stokes U (f), and polarized intensity (g) of the synthetic polarimetric observations. The red ellipse shows the synthetic beam of the simulated observations (a). For Stokes I, the contours increase as σI × 23,4,5,…. For Stokes Q and U, and PI, the contours start at 3σ and increase in steps of 1σ. Note that at σB,sp = 10 degrees a 3σ signal becomes detectable in Stokes U.
