30.23 min in both cases. The quasars which were used for calibration purposes are J0750+1231 as the flux and polarization calibrator, J0730-1141 as the phase calibrator, and J0522-3627 as the bandpass calibrator. All three quasars were also used for removal of effects of the atmosphere and pointing calibrations.\
The [*uv* ]{} data reduction was performed using the ALMA pipeline and imaging was done with The Common Astronomy Software Applications [@McMullin2007 CASA v 4.7.2]. The two executions were calibrated separately, then combined before imaging and polarization calibration. To achieve a better sensitivity and unveil more details, two rounds of self calibration were performed. We note that dynamical range of the Stokes [*I*]{} image is at best around 300 (despite the self-calibration and careful removal of the channels with line emission), indicating that all the flux is not recovered. With a maximum recoverable scale (MRS) of 3.9we have resolved out all the smooth structures larger than this size. A Briggs weighting with a robust factor of 0.5 was used to generate continuum maps with a resulting synthesized beam of 0.50$\times$0.38with a position angle PA= 85.63$\degr$. The images were also primary-beam corrected and we note that the leakage is expected to be lower 