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We present HST Planetary Camera V and I~band images of the central region ofthe peculiar giant elliptical galaxy NGC 1316. The inner profile is well fit bya nonisothermal core model with a core radius of 0.41" +/- 0.02" (34 pc). At anassumed distance of 16.9 Mpc, the deprojected luminosity density reaches $\sim2.0 \times 10^3 L_{\sun}$ 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. Theline width measurements of the center indicate the existence of either acentral dark object of mass $2 \times 10^9 M_{\sun}$, an increase in thestellar mass-to-light ratio by at least a factor of two for the inner fewarcseconds, or perhaps increasing radial orbit anisotropy towards the center.The mass-to-light ratio run in the center of NGC 1316 resembles that of manyother giant ellipticals, some of which are known from other evidence to harborcentral massive dark objects (MDO's).  We also examine twenty globular clusters associated with NGC 1316 and reporttheir brightnesses, colors, and limits on tidal radii. The brightest clusterhas a luminosity of $9.9 \times 10^6 L_{\sun}$ ($M_V = -12.7$), and thefaintest 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 coreradii 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 mergerin the recent past, young globular clusters are not detected.Comment: 21 pages, latex, postscript figures available at  ftp://delphi.umd.edu/pub/outgoing/eshaya/fornax

Hubble Space Telescope Planetary Camera Images of NGC 1316 (Fornax A)