Table 5.
Extinction within the MW towards the sample SNe.
| SN | E(B − V)MW | Pmax, MW | P(6000) |
|---|---|---|---|
| (%) | (%) | ||
| SN 2017gmr | 0.024 | 0.216 | 0.33 |
| SN 2017ahn | 0.069 | 0.621 | 0.65 |
| SN 2013ej | 0.062 | 0.558 | 0.84 |
| SN 2012ec | 0.023 | 0.207 | 0.14 |
| SN 2012dh | 0.064 | 0.576 | 0.43 |
| SN 2012aw | 0.024 | 0.216 | 0.65 |
| SN 2010hv | 0.026 | 0.234 | 0.0 |
| SN 2010co | 0.053 | 0.477 | 1.15 |
| SN 2008bk | 0.017 | 0.153 | 0.24 |
| SN 2001du | 0.018 | 0.162 | 0.17 |
| SN 2001dh | 0.052 | 0.468 | 0.56 |
Notes. The values of the extinction were taken from Schlafly & Finkbeiner (2011) through NED (NASA/IPAC Extragalactic Database; https://ned.ipac.caltech.edu). The maximum values of the ISP were calculated using the empirical relation, P ≤ 9E(B − V), from Serkowski et al. (1975). The polarization degree at 6000 Å in the best-fit ISP (see Table 4) is shown as P(6000).
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