  The prototype for events that we call MFs - "March Fifth" events or "Magnetar
Flares" - was observed on March 5, 1979. There is evidence that MFs are powered
by catastrophic magnetic instabilities in ultramagnetized neutron stars. These
events begin with brief (~ 0.1 - 1 s), intense, hard spikes of gamma rays
followed by long (~ 100 s) softer tails of hard X-rays, modulated on the
stellar rotation period. Prototypical MFs could have been detected by BATSE out
to ~ 13 Mpc, nearly reaching the Virgo cluster. The likely number of isotropic,
standard-candle MFs detected by the BATSE experiment is ~ 12. Bayes' Theorem
implies that there is a 99% chance for at least 1 MF in the BATSE catalog, and
a 16% chance for more than 20. These short-duration, fast-rising gamma-ray
bursts could in principle be identified by their positional coincidences with
nearby galaxies. The ensuing soft tail emission would not have been detected by
BATSE for sources more distant than M31.
  It is possible that MFs also emit an intense, hard, BEAMED component during
the intial spike phase. If this beamed component has opening angle ~ 8 degrees
and peak luminosity comparable to the power of the isotropic component, then
BATSE would detect such beamed sources out to redshift z ~ 0.1, at a full-sky
rate of ~ 100 yr^-1. We speculate that such beamed MFs could account for the
short, hard Class II gamma-ray bursts in the BATSE catalog, or some significant
subset of them. If true, then Class II GRBs positions would correlate with the
positions of galaxies and galaxy clusters within ~ 350 Mpc.
