Light Curve Modeling of the Type Ic Supernova 1997ef

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Abstract
The optical properties of core collapse supernovae from relatively massive C+O star progenitors are studied as a possible model for the recent Type Ic supernova 1997ef. The light curve of SN 1997ef has a broad maximum lasting (\sim) 25 days and an exponential tail declining as slow as (^{56})Co decay, and is found to be well reproduced by the explosion of a C+O star of 6 (\pm) 1.5 \ms with a kinetic energy of (1.0^{+0.9}_{-0.6} \times 10^{51}) ergs. The evolution of the overall spectral shape is also in a qualitatively good agreement with the prediction of the same model. With a distance of 52.3 Mpc and no reddening to the parent galaxy UGC4107, the inferred mass of ejected (^{56})Ni turns out to be (0.15 \pm 0.03) \ms and a small amount of mixing out (^{56})Ni is favored from the point of view of the light curve. This is an interesting case suggesting that Type Ic supernovae (SNe Ic) can be `fast' like SN 1994I but also `slow'. These latter objects seem to originate from more massive progenitors.

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