  Previous detections of an X-ray emission line near 3.5 keV in galaxy clusters
and other dark matter-dominated objects have been interpreted as observational
evidence for the decay of sterile neutrino dark matter. Motivated by this, we
report on a search for a 3.5 keV emission line from the Milky Way's galactic
dark matter halo with HaloSat. As a single pixel, collimated instrument,
HaloSat observations are impervious to potential systematic effects due to
grazing incidence reflection and CCD pixelization, and thus may offer a check
on possible instrumental systematic errors in previous analyses. We report
non-detections of a $\sim$3.5 keV emission line in four HaloSat observations
near the Galactic Center. In the context of the sterile neutrino decay
interpretation of the putative line feature, we provide 90% confidence level
upper limits on the 3.5 keV line flux and 7.1 keV sterile neutrino mixing
angle: $F \leq 0.077$ ph cm$^{-2}$ s$^{-1}$ sr$^{-1}$ and $\sin^2(2\theta) \leq
4.25 \times 10^{-11}$. The HaloSat mixing angle upper limit was calculated
using a modern parameterization of the Milky Way's dark matter distribution,
and in order to compare with previous limits, we also report the limit
calculated using a common historical model. The HaloSat mixing angle upper
limit places constraints on a number of previous mixing angle estimates derived
from observations of the Milky Way's dark matter halo and galaxy clusters, and
excludes several previous detections of the line. The upper limits cannot,
however, entirely rule out the sterile neutrino decay interpretation of the 3.5
keV line feature.
