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Fig. 2


Channel maps of the 13CH3OH(121,11–120,12)A (upper panels) and CH2DOH(162,15–161,15)o1 (lower panels) blue- and redshifted (continuum subtracted) emissions observed during ALMA-Cycle 4 towards the HH212 mm protostar. Each panel shows the emission integrated over a velocity interval of 1 km s-1 shifted with respect to the systemic velocity (see the magenta channel, sampling the velocity between +1.5 km s-1 and +2.5 km s-1) by the value given in the upper-right corner. The black cross (inclined in order to point the SiO jet direction and consequently the equatorial plane, see Fig. 1) indicates the position of the protostar. The ellipse in the top left panel shows the ALMA synthesised beam (HPBW): (PA = –88°). First contours and steps correspond to 3σ (2.7 mJy beam -1 km s-1). Note that for CH2DOH at velocities higher than +1.0 km s-1 a further emission appears along the jet axes to the north and to the south with respect to the CH2DOH emission. This is due to the SO2(82,6–71,7) emission line (see Table 1 and Fig. 2), which has been confirmed to be a good tracer of outflowing material (Podio et al. 2015). Given that the velocity scale has been derived by first fixing the CH2DOH frequency, the SO2 emission looks artificially red, but it is clearly blueshifted (see Fig. A.1).

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