  The dynamical friction timescale of massive globular clusters (GCs) in the
inner regions of cuspy dark haloes in dwarf spheroidal (dSph) galaxies can be
much shorter than the Hubble time. This implies that a small fraction of the
GCs is expected to be caught close to the centre of these galaxies. We compare
the radial distribution of GCs predicted in simple Monte Carlo models with that
of a sample of $38$ spectroscopically confirmed GCs plus 17 GC candidates,
associated mainly to low-luminosity dSph galaxies. If dark matter haloes follow
an NFW profile, the observed number of off-center GCs at projected distances
less than one half the galaxy effective radius is significantly higher than
models predict. This timing problem can be viewed as a fine-tuning of the
starting GC distances. As a result of the short sinking timescale for GCs in
the central regions, the radial distribution of GCs is expected to evolve
significantly during the next 1-2 Gyr. However, dark matter haloes with cores
of size comparable to the galaxy effective radii can lead to a slow orbital
in-spiral of GCs in the central regions of these galaxies, providing a simple
solution to the timing problem. We also examine any indication of mass
segregation in the summed distribution of our sample of GCs.
