Fig. 1
The dust at 178 GHz around of VY CMa. Arrows indicate dust clump C and the star (VY) identified in previous ALMA observations (Richards et al. 2014, OG+15). The grey-scale image is the linearly polarised intensity, which is seen to peak at the bright dust component clump C in the South-East. The black contours are the total intensity at 0.01,0.02,0.04,0.08,0.16,0.32, and 0.64 times the peak brightness. The similarly spaced red contours (left) indicate the ALMA 658 GHz continuum from OG+15. The vectors (right) indicate the direction of polarisation rotated by 90° to indicate the magnetic field direction if the polarised emission originates from magnetically aligned grains. The beam size is indicated in the lower left corner.
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