  We report measurements of the sky-projected spin-orbit angle for AU\,Mic\,b,
a Neptune-size planet orbiting a very young ($\sim20$\,Myr) nearby pre-main
sequence M dwarf star which also hosts a bright, edge-on, debris disk. The
planet was recently discovered from preliminary analysis of radial velocity
observations and confirmed to be transiting its host star from photometric data
from the NASA's \textit{TESS} mission. We obtained radial velocity measurements
of AU\,Mic over the course of two partially observable transits and one full
transit of planet b from high-resolution spectroscopic observations made with
the {\textsc{Minerva}}-Australis telescope array. Only a marginal detection of
the Rossiter--McLaughlin effect signal was obtained from the radial velocities,
in part due to AU Mic being an extremely active star and the lack of full
transit coverage plus sufficient out-of-transit baseline. As such, a precise
determination of the obliquity for AU\,Mic\,b is not possible in this study and
we find a sky-projected spin-orbit angle of $\lambda =
47{^{+26}_{-54}}^{\circ}$. This result is consistent with both the planet's
orbit being aligned or highly misaligned with the spin-axis of its host star.
Our measurement independently agrees with, but is far less precise than
observations carried out on other instruments around the same time that measure
a low obliquity orbit for the planet. AU\,Mic is the youngest exoplanetary
system for which the projected spin-orbit angle has been measured, making it a
key data point in the study of the formation and migration of exoplanets --
particularly given that the system is also host to a bright debris disk.
