  Satellite galaxies can be used to indicate the dynamical mass of galaxy
groups and clusters. In this study, we apply the axis-symmetric Jeans
Anisotropic Multi-Gaussian Expansion JAM modeling to satellite galaxies in 28
galaxy clusters selected from the TNG300-1 simulation with halo mass of
$\log_{10}M_{200}/M_\odot>14.3$. If using true bound satellites as tracers, the
best constrained total mass within the half-mass radius of satellites,
$M(<r_\mathrm{half})$, and the virial mass, $M_{200}$, have average biases of
-0.01 and $0.03$~dex, with average scatters of 0.11~dex and 0.15~dex. If
selecting companions in redshift space with line-of-sight depth of 2,000~km/s,
the biases are -0.06 and $0.01$~dex, while the scatters are 0.12 and 0.18~dex
for $M(<r_\mathrm{half})$ and $M_{200}$. By comparing the best-fitting and
actual density profiles, we find $\sim$29% of best-fitting density profiles
show very good agreement with the truth, $\sim$32% display over or under
estimates at most of the radial range with biased $M(<r_\mathrm{half})$, and
39% show under/over estimates in central regions and over/under estimates in
the outskirts, with good constraints on $M(<r_\mathrm{half})$, yet most of the
best constraints are still consistent with the true profiles within 1-$\sigma$
statistical uncertainties for the three circumstances. Using a mock DESI Bright
Galaxy Survey catalog with the effect of fiber incompleteness, we find DESI
fiber assignments and the choice of flux limits barely modify the velocity
dispersion profiles and are thus unlikely to affect the dynamical modeling
outcomes. Our results show that with current and future deep spectroscopic
surveys, JAM can be a powerful tool to constrain the underlying density
profiles of individual massive galaxy clusters.
