  We present HST Planetary Camera V and I~band images of the central region of
the peculiar giant elliptical galaxy NGC 1316. The inner profile is well fit by
a nonisothermal core model with a core radius of 0.41" +/- 0.02" (34 pc). At an
assumed distance of 16.9 Mpc, the deprojected luminosity density reaches $\sim
2.0 \times 10^3 L_{\sun}$ pc$^{-3}$.
  Outside the inner two or three arcseconds, a constant mass-to-light ratio of
$\sim 2.2 \pm 0.2$ is found to fit the observed line width measurements. The
line width measurements of the center indicate the existence of either a
central dark object of mass $2 \times 10^9 M_{\sun}$, an increase in the
stellar mass-to-light ratio by at least a factor of two for the inner few
arcseconds, or perhaps increasing radial orbit anisotropy towards the center.
The mass-to-light ratio run in the center of NGC 1316 resembles that of many
other giant ellipticals, some of which are known from other evidence to harbor
central massive dark objects (MDO's).
  We also examine twenty globular clusters associated with NGC 1316 and report
their brightnesses, colors, and limits on tidal radii. The brightest cluster
has a luminosity of $9.9 \times 10^6 L_{\sun}$ ($M_V = -12.7$), and the
faintest detectable cluster has a luminosity of $2.4 \times 10^5 L_{\sun}$
($M_V = -8.6$). The globular clusters are just barely resolved, but their core
radii are too small to be measured. The tidal radii in this region appear to be
$\le$ 35 pc. Although this galaxy seems to have undergone a substantial merger
in the recent past, young globular clusters are not detected.
