  We investigate the effects of prior selection on the inferred mass and spin
parameters of the neutron star-black hole merger GW230529\_181500.
Specifically, we explore models motivated by astrophysical considerations,
including massive binary and pulsar evolution. We examine mass and spin
distributions of neutron stars constrained by radio pulsar observations,
alongside black hole spin observations from previous gravitational wave
detections. We show that the inferred mass distribution highly depends upon the
spin prior. Specifically, under the most restrictive, binary stellar evolution
models, we obtain narrower distributions of masses with a black hole mass of
$4.1^{+0.2}_{-0.3} \,M_\odot$ and neutron star mass of $1.3^{+0.1}_{-0.1}
\,M_\odot$ where, somewhat surprisingly, it is the prior on component spins
which has the greatest impact on the inferred mass distributions. Re-weighting
using neutron star mass and spin priors from observations of radio pulsars,
with black hole spins from observations of gravitational waves, yields the
black hole and the neutron star masses to be $3.8^{+0.5}_{-0.6} \,M_\odot$ and
$1.4^{+0.2}_{-0.1} \,M_\odot$ respectively. The sequence of compact object
formation -- whether the neutron star or the black hole formed first -- cannot
be determined at the observed signal-to-noise ratio. However, there is no
evidence that the black hole was tidally spun up.
