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L_{\rm peak} \sim E_{\rm p} t_{\rm p}/t_{\rm d}^2 \sim 5 \times 10^{43} B_{14}^{-2} \kappa_{\rm es}^{-1} M_{5}^{-3/2}E_{51}^{1/2} \ \rm erg s^{-1}   \end{equation}  where $\kappa_{\rm es}$ is the electron scattering opacity, $M_{5}$ is the ejecta mass in the $5 \ M_{\odot}$ unit.  This exceeds $10^{43} \rm \ erg \ s^{-1} $, making these events brighter than normal core-collapse Type II-P SNe. Figure 4 and 5 in \citet{Kasen_2010} show the dependence of the  peak luminosity and the  time to peak on $B$ and $P_i$ for ejecta mass of $5$ and $20 \ M_{\odot}$ respectively. If magnetars with different magnetic field strengths and birth periods are responsible for both LGRBs and SLSNe, at least some LGRBs should be accompanied by SNe. These associations between GRBs and SNe are indeed observed, with the first pair of events being SN\,1998bw and GRB 980425 \cite{Kulkarni_1998}. A number of other events have since been observed (see e.g. \citealp{Woosley_2006} for a review). \citet{Metzger_2015} showed that magnetars in the transition region in the $B-P_i$ plane with $P_i \sim 2 \ \rm ms$ and the spin-down timescale of $\sim 10^4 \ \rm s$  can explain GRB 111209 and SN\,2011kl pair and the SLSN ASASSN-15lh, the most luminous SN ever observed. This association between GRBs and SNe is another evidence that these two classes of events share magnetar as their central engine. As modern transients surveys in all wavelengths continue to discover various types of peculiar events, we will have more data to constrain theoretical models, leading to a better understanding of this messy ending chapter of the stellar evolution.