  We present updated results constraining multiplicity demographics for the
stellar population of the Orion Nebula Cluster (ONC, a high-mass, high-density
star-forming region), across primary masses 0.08-0.7M$_{\odot}$. Our study
utilizes archival Hubble Space Telescope data obtained with the Advanced Camera
for Surveys using multiple filters (GO-10246). Previous multiplicity surveys in
low-mass, low-density associations like Taurus identify an excess of companions
to low-mass stars roughly twice that of the Galactic field and find the mass
ratio distribution consistent with the field. Previously, we found the
companion frequency to low-mass stars in the ONC is consistent with the
Galactic field over mass ratios=0.6-1.0 and projected separations=30-160au,
without placing constraints on the mass ratio distribution. In this study, we
investigate the companion population of the ONC with a double point-spread
function (PSF) fitting algorithm sensitive to separations larger than 10au
(0.025") using empirical PSF models. We identified 44 companions (14 new), and
with a Bayesian analysis, estimate the companion frequency to low-mass stars in
the ONC =0.13$^{+0.05}_{-0.03}$ and the power law fit index to the mass ratio
distribution =2.08$^{+1.03}_{-0.85}$ over all mass ratios and projected
separations of 10-200au. We find the companion frequency in the ONC is
consistent with the Galactic field population, likely from high transient
stellar density states, and a probability of 0.002 that it is consistent with
that of Taurus. We also find the ONC mass ratio distribution is consistent with
the field and Taurus, potentially indicative of its primordial nature, a direct
outcome of the star formation process.
