Modeling the Light Curves of the Luminous Type Ic Supernova 2007D

Abstract

SN~2007D is a nearby (redshift $z=0.023146$), luminous Type Ic supernova (SN) having a narrow light curve (LC) and high peak luminosity. Previous research based on the assumption that it was powered by the ${}^{56}$Ni cascade decay suggested that the inferred ${}^{56}$Ni mass and the ejecta mass are $\sim 1.5$M${}_{\odot }$ and $\sim 3.5$M${}_{\odot }$, respectively. In this paper, we employ some multiband LC models to model the $R$-band LC and the color ($V-R$) evolution of SN~2007D to investigate the possible energy sources powering them. We find that the pure ${}^{56}$Ni model is disfavored; the multiband LCs of SN~2007D can be reproduced by a magnetar whose initial rotational period $P_0$ and magnetic field strength $B_p$ are $7.28_{-0.21}^{+0.21}$ (or $9.00_{-0.42}^{+0.32}$) ms and $3.10_{-0.35}^{+0.36}\times 10^{14}$ (or $2.81_{-0.44}^{+0.43}\times 10^{14}$) G, respectively. By comparing the spectrum of SN~2007D with that of some superluminous SNe (SLSNe), we find that it might be a luminous SN like several luminous ``gap-filler" optical transients that bridge ordinary and SLSNe, rather than a genuine SLSN.

arXiv comment11 pages, 5 figures, 1 table, accepted for publication in ApJ

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