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Context. Globular clusters (GCs) carry information about the formationhistories and gravitational fields of their host galaxies. B\'ilek et al.(2019, BSR19 hereafter) reported that the radial profiles of the volume numberdensity of GCs in GC systems (GCSs) follow broken power laws, while the breaksoccur approximately at the a0 radii. These are the radii at which thegravitational fields of the galaxies equal the galactic acceleration scale $a_0= 1.2\times 10^{-10}$ms$^{-2}$ known from the radial acceleration relation orthe MOND theory of modified dynamics.  Aims. Our main goals here are to explore whether the results of BSR19 holdtrue for galaxies of a wider mass range and for the red and blue GCsubpopulations.  Methods. We exploited catalogs of photometric GC candidates in the Fornaxgalaxy cluster based on ground and space observations and a new catalog ofspectroscopic GCs of NGC 1399, the central galaxy of the cluster. For everygalaxy, we obtained the parameters of the broken power-law density by fittingthe on-sky distribution of the GC candidates, while allowing for a constantdensity of contaminants. The logarithmic stellar masses of our galaxy samplespan 8.0 - 11.4$M_\odot$.  Results. All investigated GCSs with a sufficient number of members showbroken power-law density profiles. This holds true for the total GC populationand the blue and red subpopulations. The inner and outer slopes and the breakradii agree well for the different GC populations. The break radii agree withthe 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 galacticstellar masses. The break radii of NGC 1399 vary in azimuth, such that they aregreater toward and against the interacting neighbor galaxy NGC 1404.

The galactic acceleration scale is imprinted on globular cluster systems  of early-type galaxies of most masses and on red and blue globular cluster  subpopulations