Fig. 11
Velocity evolution ofFe ii lines in SN 2012aa. The three linesFe ii λλ4924, 5018, 5169 are difficult to identify unambiguously. We found two different possibilities in SN 2012aa, shown here using the +50 d spectrum; the lines are respectively marked with blue, orange, and red arrows in the insets. Lower panel: the velocity evolution is a power law common in CCSNe. Upper panel: the velocity evolution has a shallow decline common in SLSNe.
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