tokens: Right panels present the distributions of the position angles of the magnetic field orientations as a function of distance from the protostars. If multiple protostars are present in one core, the distances between the magnetic field orientations and the protostar closest to the Stokes I intensity peak are calculated. In the middle and right panels, black dashed lines denote the mean magnetic field orientations computed from the averaged Stokes Q and U emission in the area of the dense cores, and red solid and dashed–dotted (if there are multiple outflows) lines show the position angles of the outflows. The names of the protostars are labeled in the order from western to eastern sources above the middle panel in each row. Figure 12.16. L1157 Same as Figures 3 and 4, but left panels only present the magnetic orientations (small orange segments) detected in the 40′′ × 40′′ regions (dashed open squares) around the sample protostars as well as the mean orientations of the magnetic field (long thick orange segments) in the individual dense cores/clumps. Left panels show the Stokes I maps (gray scale) of the dense cores, where the sample protostars are embedded, and green contours delineate the area of the dense cores identified by Clumpf ind . Yellow dots show the locations of the protostars, and blue and red arrows present the orientations of their blue- and redshifted outflows. Black horizontal segments denote the spatial scale of 0.02 pc (or ∼4000 au). Middle panels present the distributions of the position angles of the individual magnetic field orientations detected with the JCMT POL-2 observations. Right panels present the distributions of the position angles of the magnetic field orientations as a function of distance from the protostars. If multiple protostars are present in one core, the distances between the magnetic field orientations and the protostar closest to the Stokes I intensity peak are calculated. In the middle and right panels, black dashed lines denote the mean magnetic field orientations computed from the averaged Stokes Q and U emission in the area of the dense cores, and red solid and dashed–dotted (if there are multiple outflows) lines show the position angles of the outflows. The names of the protostars are labeled in the order from western to eastern sources above the middle panel in each row. Appendix D Dependences of Misalignment on Source Properties Figure 13 compares the measured misalignment angles with the sizes, total fluxes, mean intensities, and mean polarization percentages of the dense cores and the distances to the sources. The total flux and mean intensity are expected to be proportional to the total mass and mean column density of a dense core, respectively. These comparisons show that the measured misalignments do not depend on the mass and density of the dense cores. We note that the magnetic field structures in the nearby sources can be better resolved than in the distant sources. The comparison also
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