Image Details
Caption: Figure 11.
Rotationally symmetric linear polarization structure as a function of spin, encapsulated in the phase and amplitude of β 2. For this plot, MAD R high = 10, i = 30°/150° reversed models are included, with either i = 30° in blue or i = 150° in red. Our observational constraints are shown as gray bands, and the constraint prior to RM derotation is shown as a hatched region. In this slice of parameter space, prograde models with spin values that are too large tend to produce polarization patterns that are too azimuthally symmetric and radially oriented compared to our observations.
© 2024. The Author(s). Published by the American Astronomical Society.