  Due to observational challenges, the mass function of black holes (BH) at
lower masses is poorly constrained in the local universe. Understanding the
occupation fraction of BHs in low-mass galaxies is crucial for constraining the
origins of supermassive BH seeds. Compact stellar systems (CSSs), including
ultra-compact dwarf galaxies (UCDs) and compact elliptical galaxies (cEs), are
potential intermediate-mass BH hosts. Despite the difficulties posed by their
limited spheres of influence, stellar dynamical modeling has been effective in
estimating central BH masses in CSSs. Some CSSs may harbor a BH constituting up
to 20% of their host stellar mass, while others might not have a central BH. In
support of our ongoing efforts to determine the BH masses in select CSSs in the
Virgo cluster using JWST/NIRSpec IFU observations and orbit-superposition
dynamical models, we create mock kinematic data mimicking the characteristics
of observed cEs/UCDs in the Virgo cluster with different BH masses. We then
construct a series of dynamical models using the orbit-superposition code
FORSTAND and explore the accuracy of recovering the BH mass. We find that the
mass of BHs comprising 1% or more of the total host stellar mass can be
accurately determined through kinematic maps featuring higher-order velocity
moments. We also assess how BH mass measurement is affected by deprojection
methods, regularization factors, anisotropy parameters, orbit initial
conditions, the absence of higher-order velocity moments, spatial resolution,
and the signal-to-noise ratio.
