Image Details
Caption: Figure 1.
(a) The overall structure of the B213 filament is shown using a high-resolution (18.″2) column density map taken from the HGBS archive (Palmeirim et al. 2013). It is a part of the 10 pc long large-scale filament LDN 1495 in the Taurus molecular cloud. Measurements of the large-scale B-field orientation are overlaid: optical polarimetry measurements are shown as magenta segments (Heyer et al. 1987; Goodman et al. 1990; Heiles 2000), NIR polarimetry measurements as cyan segments (Goodman et al. 1992; Chapman et al. 2011), and Planck 850 μm dust emission polarimetry measurements as yellow segments. (b) Our inferred core-scale B-field geometry (red segments) superimposed on the area of our total intensity (Stokes I) map, which contains the fragmented cores of B213. The extent of the map is shown as a white box in panel (a). Plotted segments correspond to a detection at a minimum of 3σ in polarization fraction and 10σ in total intensity. Note that all segments are shown with equal lengths to better display the B-field morphology. The white contour marks a column density of 1 × 1022 cm−2 (Palmeirim et al. 2013), as measured in the Herschel data, that outlines the structure of the parental B213 filament, which has fragmented into the cores shown. Red contours in both panels mark 10σ total intensity (Stokes I) values, where 1σ = 1.3 mJy beam−1 is the rms noise. Note that the apparent >10σ intensity values seen in low column density regions in panel (a) result from low exposure times at the edges of the POL-2 map and so delineate the extent of our mapped area. Reference scale and beam size (∼14.″1) are shown.
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© 2021. The Author(s). Published by the American Astronomical Society.
