  We present a new wide field image of the distant cluster AC114 ($z=0.31$)
obtained with Wide Field and Planetary Camera II onboard the Hubble Space
Telescope. This image considerably extends our knowledge of the lensing
properties of the cluster beyond those derived by Smail \et (1995a) from a
single WF/PC-1 pointing. In conjunction with published ground-based
spectroscopy, we utilise several newly-discovered multiple images to construct
an improved mass model for the central regions of the cluster. Using this
model, we apply the methodology introduced by Natarajan & Kneib (1997) to
interpret local perturbations to the cluster shear field on small scales
resulting from mass associated with individual cluster galaxies. We use the
lensing signal to place new constraints on the average mass-to-light ratio and
spatial extents of the dark matter halos associated with
morphologically-classified early-type cluster members. We find that the total
mass of a fiducial $L^*$ cluster spheroidal galaxy is largely contained within
$\sim$ 15 kpc radius halo ($\sim$~8--10 $R_e$) with a mass-to-light ratio
${M/L_V} \sim {15^{+10}_{-4}} $ (90% c.l., $h=0.5$) in solar units within this
radius. Comparisons with similar estimates for fieldgalaxies indicates that the
cluster galaxies in AC114 may possess less extensive and less massive halos. We
discuss the consequences of our result in the context of models for the
dynamical evolution of cluster galaxies and the observational prospects for
extending this analysis.
