Polarization signatures of a high-velocity scatterer in nebular-phase spectra of Type II supernovae

Open Access

Fig. E.2

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Same as Fig. E.1, but all calculations are now done at a much later time in the nebular phase, namely 527 d after explosion. Top panel: equivalent of Fig. E.1 at that older time. Bottom panel: P_cont ∕(cos_β sin²β) versus inclination. In both panels, the dashed line gives the analytic prediction.

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