  A very massive star with a carbon-oxygen core in the range of $64$
M$_{\odot}<M_{\mathrm{CO}}<133$ M$_{\odot}$ is expected to undergo a very
different kind of explosion known as a pair instability supernova. Pair
instability supernovae are candidates for superluminous supernovae due to the
prodigious amounts of radioactive elements they create. While the basic
mechanism for the explosion is understood, how a star reaches a state is not,
thus observations of a nearby pair-instability supernova would allow us to test
current models of stellar evolution at the extreme of stellar masses. Much will
be sought within the electromagnetic radiation we detect from such a supernova
but we should not forget that the neutrinos from a pair-instability supernova
contain unique signatures of the event that unambiguously identify this type of
explosion. We calculate the expected neutrino flux at Earth from two,
one-dimensional pair-instability supernova simulations which bracket the mass
range of stars which explode by this mechanism taking into account the full
time and energy dependence of the neutrino emission and the flavor evolution
through the outer layers of the star. We calculate the neutrino signals in five
different detectors chosen to represent present or near future designs. We find
the more massive progenitors explode as pair-instability supernova which can
easily be detected in multiple different neutrino detectors at the `standard'
supernova distance of $10\;{\rm kpc}$ producing several events in DUNE, JUNE
and SuperKamiokande, while the lightest progenitors only produce a handful of
events (if any) in the same detectors. The proposed HyperKamiokande detector
would detect neutrinos from a large pair-instability supernova as far as $\sim
50\;{\rm kpc}$ allowing it to reach the Megallanic Clouds and the several very
high mass stars known to exist there.
