Fig. C.1.
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Example NOT/ALFOSC polarimetry images for SN 2017egm, SN 2018bgv, SN 2018ffj, SN 2019neq and SN 2020tcw. In the polarimetric mode, the e (left) and o beams (right) are overlaid with an offset of 15″. In addition to the SNe, bright point sources (i.e. stars) have been marked in the images. For SN 2017egm, Star 1 is located on the edge of the e beam image and is unreliable to estimate the ISP. No stars are present in the FOV of SN 2018bgv. Star 1 was used to estimate the ISP for SN 2018ffj. For SN 2019neq, only Star 2 is used to determine the ISP as Star 1 is found on the edge of the o beam image resulting in an unreliable ISP estimate. Only Star 1 is used to estimate the ISP of SN 2020tcw as Star 2 has several objects in the close vicinity and the ISP cannot be reliably identified.
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