  In May 2023, the LIGO Livingston observatory detected the likely black
hole-neutron star (BHNS) merger GW230529_181500. That event is expected to be
the merger of a 2.5-4.5 $M_{\odot}$ primary with a secondary compact object of
mass between 1.2-2.0 $M_{\odot}$. This makes it the first BHNS merger with a
significant potential for the production of electromagnetic (EM) counterparts,
and provides further evidence for compact objects existing within the suspected
lower mass gap. To produce post-merger EM transients, the component of the
black hole spin aligned with the orbital angular momentum must be sufficiently
high, allowing the neutron star to be tidally disrupted. The disrupting BHNS
binary may then eject a few percent of a solar mass of matter, leading to an
observable kilonova driven by radioactive decays in ejecta, and/or a
compact-binary GRB (cbGRB) resulting from the formation of an accretion disk
and relativistic jet. Determining which mergers lead to disruption of the
neutron star is necessary to predict the prevalence of EM signals from BHNS
mergers, yet most BHNS simulations so far have been performed far from the
minimum spin required for tidal disruption. Here, we use the Spectral Einstein
Code (SpEC) to explore the behavior of BHNS mergers in a mass range consistent
with GW230529_181500 close to that critical spin, and compare our results
against the mass remnant model currently used by the LVK collaboration to
predict the probability of tidal disruption. Our numerical results reveal the
emergence of non-zero accretion disks even below the predicted NS disruption
limit, of low mass but capable of powering cbGRBs. Our results also demonstrate
that the remnant mass model underpredicts the disk mass for the DD2 EOS, while
they are within expected modeling errors for SFHo. In all of our simulations,
any kilonova signal would be dim and dominated by post-merger disk outflows.
