  The presence or absence of intermediate-mass black holes (IMBHs) at the
centre of Milky Way globular clusters (GCs) is still an open question. This is
either due to observational restrictions or limitations in the dynamical
modelling method; in this work, we explore the latter. Using a sample of
high-end Monte Carlo simulations of GCs, with and without a central IMBH, we
study the limitations of spherically symmetric Jeans models assuming constant
velocity anisotropy and mass-to-light ratio. This dynamical method is one of
the most widely used modelling approaches to identify a central IMBH in
observations.
  With these models, we are able to robustly identify and recover the mass of
the central IMBH in our simulation with a high-mass IMBH ($M_{\rm IMBH}/M_{\rm
GC}\sim4\%$). Simultaneously, we show that it is challenging to confirm the
existence of a low-mass IMBH ($M_{\rm IMBH}/M_{\rm GC}\sim0.3\%$), as both
solutions with and without an IMBH are possible within our adopted error bars.
For simulations without an IMBH we do not find any certain false detection of
an IMBH. However, we obtain upper limits which still allow for the presence of
a central IMBH. We conclude that while our modelling approach is reliable for
the high-mass IMBH and does not seem to lead towards a false detection of a
central IMBH, it lacks the sensitivity to robustly identify a low-mass IMBH and
to definitely rule out the presence of an IMBH when it is not there.
