  The discovery of 150 - 300 M$_{\odot}$ stars in the Local Group and
pair-instability supernova candidates at low redshifts has excited interest in
this exotic explosion mechanism. Realistic light curves for pair-instability
supernovae at near-solar metallicities are key to identifying and properly
interpreting these events as more are found. We have modeled pair-instability
supernovae of 150 - 500 M$_{\odot}$ Z $\sim$ 0.1 - 0.4 Z$_{\odot}$ stars. These
stars lose up to 80% of their mass to strong line-driven winds and explode as
bare He cores. We find that their light curves and spectra are quite different
from those of Population III pair-instability explosions, which therefore
cannot be used as templates for low-redshift events. Although non-zero
metallicity pair-instability supernovae are generally dimmer than their
Population III counterparts, in some cases they will be bright enough to be
detected at the earliest epochs at which they can occur, the formation of the
first galaxies at $z \sim$ 10 - 15. Others can masquerade as dim, short
duration supernovae that are only visible in the local universe and that under
the right conditions could be hidden in a wide variety of supernova classes. We
also report for the first time that some pair-instability explosions can create
black holes with masses of $\sim$ 100 M$_{\odot}$.
