A Population of Non-Recycled Pulsars Orginating in Globular Clusters
  We explore the enigmatic population of long-period, apparently non-recycled
pulsars in globular clusters, building on recent work by Boyles et al (2011).
This population is difficult to explain if it formed through typical core
collapse supernovae, leading many authors to invoke electron capture
supernovae. Where Boyles et al. dealt only with non-recycled pulsars in
clusters, we focus on the pulsars that originated in clusters but then escaped
into the field of the Galaxy due to the kicks they receive at birth. The
magnitude of the kick induced by electron capture supernovae is not well known,
so we explore various models for the kick velocity distribution and size of the
population. The most realistic models are those where the kick velocity is <~
10 km/s and where the number of pulsars scales with the luminosity of the
cluster (as a proxy for cluster mass). This is in good agreement with other
estimates of the electron capture supernovae kick velocity. We simulate a
number of large-area pulsar surveys to determine if a population of pulsars
originating in clusters could be identified as being separate from normal disk
pulsars. We find that the spatial and kinematical properties of the population
could be used, but only if large numbers of pulsars are detected. In fact, even
the most optimistic surveys carried out with the future Square Kilometer Array
are likely to detect < 10% of the total population, so the prospects for
identifying these as a separate group of pulsars are presently poor.
