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To assess the effectiveness of optical emission as a probe of spatialasymmetry in core-collapse supernovae (CCSNe), we apply the radiative transfersoftware, \supernu, to a unimodal CCSN model. The \snsph\radiation-hydrodynamics software was used to simulate an asymmetric explosionof a 16 M$_{\odot}$ ZAMS binary star. The ejecta has 3.36 M$_{\odot}$ with0.024 M$_{\odot}$ of radioactive $^{56}$Ni, with unipolar asymmetry along thez-axis. For 96 discrete angular views, we find the ratio between maximum andminimum peak total luminosities is $\sim$1.36. The brightest light curvesemerge from views orthogonal to the z-axis. Multigroup spectra from UV to IRare obtained. We find a shift in wavelength with viewing angle in a near-IR CaII emission feature, consistent with Ca being mostly in the unimode. We compareemission from the grey gamma-ray transfer in \supernu\ and from the detailedgamma-ray transfer code \maverick. Relative to the optical light curves, thebrightness of the gamma-ray emission is more monotonic with respect to viewingangle. UBVRI broad-band light curves are also calculated. Parallel with theunimode, the U and B bands have excess luminosity at $\gtrsim 10$ dayspost-explosion, due to $^{56}$Ni on the unimode. We compare our CCSN model withSN 2002ap, which is thought to have a similar ejecta morphology.

Light Curves and Spectra from a Unimodal Core-Collapse SuperNova