  Shells in Elliptical Galaxies are faint, sharp-edged features, believed to
provide evidence of a recent ($\sim 0.5 - 2 \times 10^9$ years ago) merger
event. We analyse the Globular Cluster (GC) systems of six shell elliptical
galaxies, to examine the effects of mergers upon the GC formation history. We
examine the colour distributions, and investigate differences between red and
blue globular cluster populations. We present luminosity functions, spatial
distributions and specific frequencies ($S_N$) at 50 kpc radius for our sample.
We present V and I magnitudes for cluster candidates measured with the HST
Advanced Camera for Surveys (ACS). Galaxy background light is modelled and
removed, and magnitudes are measured in 8 pixel (0.4 arcsec) diameter
apertures. Background contamination is removed using counts from HDFS. We find
that the colour distributions for NGC 3923 and NGC 5982 have a bimodal form
typical of bright ellipticals, with peaks near $V-I=0.92 \pm 0.04$ and
$V-I=1.18 \pm 0.06$. In NGC 7626, we find in addition a population of
abnormally luminous clusters at $M_I=-12.5$. In NGC 2865 we find an unusually
blue population, which may also be young. In NGC1344 and NGC474 the red cluster
population is marginally detected. The radial surface density profiles are more
flattened than the galaxy light in the cores. As already known, in NGC3923,
which has a high $S_N$ of 5.6, the radial density distribution is more
shallower than the diffuse galaxy light. The clusters in NGC 2865 and NGC 7626
provide evidence for formation of a population associated with a recent merger.
In the other galaxies, the properties of the clusters are similar to those
observed in other, non-shell, elliptical galaxies.
