  Recent observations by the Fermi Large Area Telescope (LAT) and the High
Energy Stereoscopic System (H.E.S.S.) have revealed globular clusters (GC) to
be sources of high-energy (HE) and very-high-energy (VHE) gamma-rays. It has
been suggested that the presence of large numbers of millisecond pulsars (MSPs)
within these clusters may be either directly responsible for these gamma-ray
fluxes through emission of pulsed curvature radiation, or indirectly through
the injection of relativistic leptons into the cluster. These relativistic
particles are plausibly re-accelerated in shocks, created by the collision of
stellar winds, before interacting with the soft-photon radiation field set up
by the stellar population of the host cluster. Inverse Compton (IC) scattering
then produces gamma-radiation in the TeV band. In order to calculate the IC
spectrum, an accurate profile for the energy density of the soft-photon field
is required. We construct such a profile by deriving a radially-dependent
expression for the stellar energy density, and then solve it numerically. As a
next step, the average energy density values for three different regions of the
cluster (demarcated by its core, half-mass, and tidal radii) are determined,
which we consequently import into an existing radiation code to predict the TeV
gamma-ray spectrum. As an application, we consider the case of Terzan 5,
boasting a population of 34 radio MSPs, and compare our predicted spectrum with
that measured by H.E.S.S.
