  The merger of two neutron stars produces an outflow of radioactive heavy
nuclei. Within a second of merger, the central remnant is expected to also
launch a relativistic jet, which shock-heats and disrupts a portion of the
radioactive ejecta. Within a few hours, emission from the radioactive material
gives rise to an ultraviolet, optical, and infrared transient (a kilonova). We
use the endstates of a suite of 2D relativistic hydrodynamic simulations of
jet-ejecta interaction as initial conditions for multi-dimensional Monte Carlo
radiation transport simulations of the resulting viewing angle-dependent light
curves and spectra starting at 1.5h after merger. We find that on this
timescale, jet shock heating does not affect the kilonova emission. However,
the jet disruption to the density structure of the ejecta does change the light
curves. The jet carves a channel into the otherwise spheroidal ejecta,
revealing the hot, inner regions. As seen from near ($\lesssim 30 \deg$) the
jet axis, the kilonova is brighter by a factor of a few and bluer. The strength
of this effect depends on the jet parameters, since the light curves of more
heavily disrupted ejecta are more strongly affected. The light curves and
spectra are also more heavily modified in the ultraviolet than in the optical.
