  Context. Globular clusters (GCs) carry information about the formation
histories and gravitational fields of their host galaxies. B\'ilek et al.
(2019, BSR19 hereafter) reported that the radial profiles of the volume number
density of GCs in GC systems (GCSs) follow broken power laws, while the breaks
occur approximately at the a0 radii. These are the radii at which the
gravitational fields of the galaxies equal the galactic acceleration scale $a_0
= 1.2\times 10^{-10}$ms$^{-2}$ known from the radial acceleration relation or
the MOND theory of modified dynamics.
  Aims. Our main goals here are to explore whether the results of BSR19 hold
true for galaxies of a wider mass range and for the red and blue GC
subpopulations.
  Methods. We exploited catalogs of photometric GC candidates in the Fornax
galaxy cluster based on ground and space observations and a new catalog of
spectroscopic GCs of NGC 1399, the central galaxy of the cluster. For every
galaxy, we obtained the parameters of the broken power-law density by fitting
the on-sky distribution of the GC candidates, while allowing for a constant
density of contaminants. The logarithmic stellar masses of our galaxy sample
span 8.0 - 11.4$M_\odot$.
  Results. All investigated GCSs with a sufficient number of members show
broken power-law density profiles. This holds true for the total GC population
and the blue and red subpopulations. The inner and outer slopes and the break
radii agree well for the different GC populations. The break radii agree with
the a0 radii typically within a factor of two for all GC color subpopulations.
The outer slopes correlate better with the a0 radii than with the galactic
stellar masses. The break radii of NGC 1399 vary in azimuth, such that they are
greater toward and against the interacting neighbor galaxy NGC 1404.
