  Almost all galaxies along the Hubble sequence host a compact massive object
(CMO) in their center. The CMO can be either a supermassive black hole (SMBH)
or a very dense stellar cluster, also known as nuclear star cluster (NSC).
Generally, heavier galaxies (mass $\gtrsim 10^{11}\mathrm{M}_{\odot}$ ) host a
central SMBH while lighter show a central NSC. Intermediate mass hosts,
instead, contain both a NSC and a SMBH. One possible formation mechanisms of a
NSC relies on the dry-merger (migratory) scenario, in which globular clusters
(GCs) decay toward the center of the host galaxy and merge. In this framework,
the absence of NSCs in high-mass galaxies can be imputed to destruction of the
infalling GCs by the intense tidal field of the central SMBH. In this work, we
report preliminary results of N-body simulations performed using our
high-resolution, direct, code HiGPUs, to investigate the effects of a central
SMBH on a single GC orbiting around it. By varying either the mass of the SMBH
and the mass of the host galaxy, we derived an upper limit to the mass of the
central SMBH, and thus to the mass of the host, above which the formation of a
NSC is suppressed.
