  It has been recently claimed that a surprisingly massive black hole (BH) is
present in the core of the dwarf spheroidal galaxy (dSph) Leo I. Based on
integral field spectroscopy, this finding challenges the typical expectation of
dSphs hosting BHs of intermediate-mass, since such a BH would better be
classified as supermassive. Indeed, the analysis points toward Leo I harboring
a BH with a lower mass limit exceeding a few $10^6M_\odot$ at $1\sigma$, and
the no BH case excluded at 95\% significance. Such a value, comparable to the
entire stellar mass of the galaxy, makes Leo I a unique system that warrants
further investigations. Using equilibrium models based on distribution
functions (DFs) depending on actions $f({\boldsymbol J})$ coupled with the same
integral field spectroscopy data and an extensive exploration of a very large
parameter space, we demonstrate, within a comprehensive Bayesian framework of
model-data comparison, that the posterior on the BH mass is flat towards the
low-mass end and, thus, that the kinematics of the central galaxy region only
imposes an upper limit on the BH mass of few $10^5M_\odot$ (at $3\sigma$). Such
an upper limit brings back the putative BH of Leo I under the category of
intermediate-mass BHs, and it is also in line with formation scenarios and
expectations from scaling relations at the mass regime of dwarf galaxies.
