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Fig. 8


Spectral evolution for models He_R11 (left) and He_R173 (right) covering the first week after explosion. The top panels show the ultraviolet and optical ranges and the bottom panels show the region around 5875 Å; the P Cygni profile to the red of He I 5875 Å is due to He I 6678 Å. Since these ejecta models do not contain any 56Ni, the presence of He I lines is not a result of non-thermal effects (see also Dessart et al. 2011). Blue featureless spectra in Type Ib SNe are compatible with a giant progenitor star, like our model He_R173.

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