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Fig. 20


Expansion velocities measured for the SNe of our sample, derived from the position of the P Cygni minima for the following lines: Hα, Hβ, He i λ5876, Fe ii λ5169 and Sc ii λ6246. The velocities of the Balmer lines of SN 2007pk up to day +8, derived by the FWHM of the narrow emissions (cf. Table 8), are not shown here.

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