ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject B-Citation I-Citation I-Citation I-Citation O O B-CelestialObject B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: 28, 40, 56, 79, 111, 155, and where is the rms noise in Stokes I . Green line segments: magnetic field orientation (perpendicular to polarization orientation). Grayscale background: polarization fraction (%) shown with a power law (). The orange double-headed arrow shows the outflow orientation. The small, black, double-headed arrow in the bottom-right of each synthetic observation (right-hand panels) indicates the average (unweighted) magnetic field orientation. In the top row of Figure 2 , which shows the face-on view of the magnetic field, there is no clear overall magnetic field orientation. In contrast, edge-on views from the y - and x -directions (middle and bottom rows of Figure 2 , respectively) show that the magnetic field morphology is vertical when viewed from both of these orthogonal edge-on views. We have produced additional edge-on synthetic observations using intermediate values of θ (not pictured here). Due to the initial azimuthal symmetry of the simulation and the fact that the initial magnetic field is in the z -direction, we find that all edge-on views look very similar. There are also hints of the characteristic “hourglass” morphology in the edge-on views. This is similar to observations of hourglass-shaped fields in sources such as NGC 1333-IRAS 4A (Girart et al. 2006 ) and L1157 (Stephens et al. 2013 ; Hull et al. 2014 ), where gravitational collapse of a strongly magnetized protostellar core is expected to pinch magnetic field lines. 3.1. Polarization Fraction To explore projection effects, we render projected energy density maps and synthetic polarization maps at viewing angles and , where corresponds to the face-on view and corresponds to the edge-on view from the y -direction. Figure 3 shows the orthogonal viewing angles along and z . Figure 4 shows the views from , , and (top to bottom). We present the synthetic dust polarization maps in the left panel with their corresponding energy density projections on the right. Figure 3. From top to bottom: the x – y plane (face-on), x – z plane, and y – z plane (both edge-on) viewed from z , y , and x directions respectively. Left: synthetic dust polarization maps of S2.5 at , plotted in the same manner as the right-hand panels in Figure 2 . The outflow direction was not discernible in the face-on view. Right: the corresponding energy density, where high energy densities in pink indicate the location of the outflow. Figure 4. Same as Figure 3 , but for intermediate viewing angles , and , where where corresponds to the face-on view from the z -direction, and corresponds to the edge-on view from the y -direction. We calculate the average value of polarization fraction for each dust polarization map by averaging the magnitude of the polarized intensity. The average polarization fraction, , is sensitive to the weighting scheme used to derive it. Also, the locations of the peak intensities of the total and polarized emission are not the same for every source (this is the case for