  We present the $V$-band globular cluster luminosity functions (GCLFs) of the
Fornax Cluster galaxies NGC 1344, NGC 1380, NGC 1399, and NGC 1404. Our
observations reach to $V = 24.8$, roughly one magnitude beyond the GCLF
turnover $m^0_V$, with $\sim90\%$ completeness. From the amplitude of the
galaxy surface brightness fluctuations, we also estimate the number of globular
clusters fainter than this cutoff magnitude. The GCLFs of these galaxies are
well fitted by Gaussians; the weighted means of their turnover magnitudes and
dispersions are $\langle m^0_V\rangle = 23.88 \pm 0.10$ mag and
$\langle\sigma\rangle = 1.35\pm 0.07$ mag. The assumption of a universal value
for the absolute magnitude of the turnover $M^0_V$ places the Fornax cluster
$0.13 \pm 0.11$ mag more distant than Virgo. However, in light of recent
Cepheid and other high-precision distance measurements, as well as ongoing HST
observations of GCLFs for the purpose of determining the extra-galactic
distance scale, we choose to re-examine the universal GCLF hypothesis. Based on
data from groups and clusters of galaxies, we find evidence that $M^0_V$
becomes fainter as the local density of galaxies increases. We speculate on the
possible cause of this trend; if it is confirmed, GCLF observations will be
less useful for determining distances, but may provide important information
for constraining theories of star formation in primordial galaxy halos.
