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A fully 3D Monte Carlo scheme is applied to compute optical bolometric lightcurves for aspherical (jet-like) supernova explosion models. Density andabundance distributions are taken from hydrodynamic explosion models, with theenergy varied as a parameter to explore the dependence. Our models showinitially a very large degree ($\sim 4$ depending on model parameters) ofboosting luminosity toward the polar ($z$) direction relative to the equatorial($r$) plane, which decreases as the time of peak is approached. After the peak,the factor of the luminosity boost remains almost constant ($\sim 1.2$) untilthe supernova enters the nebular phase. This behavior is due mostly to theaspherical $^{56}$Ni distribution in the earlier phase and to the disk-likeinner low-velocity structure in the later phase. Also the aspherical modelsyield an earlier peak date than the spherical models, especially if viewed fromnear the z-axis. Aspherical models with ejecta mass $\sim 10\Msun$ areexamined, and one with the kinetic energy of the expansion $\sim 2 \pm 0.5\times 10^{52}$ ergs and a mass of $^{56}$Ni $\sim 0.4\Msun$ yields a lightcurve in agreement with the observed light curve of SN 1998bw (the prototypicalhyper-energetic supernova). The aspherical model is also at least qualitativelyconsistent with evolution of photospheric velocities, showing large velocitiesnear the z-axis, and with a late-phase nebular spectrum. The viewing angle isclose to the z-axis, strengthening the case for the association of SN 1998bwwith the gamma ray burst GRB980425.Comment: Accepted by the Astrophysical Journal. 28 pages, 14 figure

Optical Emission from Aspherical Supernovae and the Hypernova SN 1998bw