  The gravitational interactions between the Milky Way and in-falling
satellites offer a wealth of information about the formation and evolution of
our Galaxy. In this paper, we explore the high-dimensionality of the GALAH DR3
plus Gaia eDR3 data set to identify new tidally stripped candidate stars of the
nearby star cluster Omega Centauri ($\omega\,\mathrm{Cen}$). We investigate
both the chemical and dynamical parameter space simultaneously, and identify
cluster candidates that are spatially separated from the main cluster body, in
regions where contamination by halo field stars is high. Most notably, we find
candidates for $\omega\,\mathrm{Cen}$ scattered in the halo extending to more
than $50^{\circ}$ away from the main body of the cluster. Using a grid of
simulated stellar streams generated with $\omega\,\mathrm{Cen}$ like orbital
properties, we then compare the on sky distribution of these candidates to the
models. The results suggest that if $\omega\,\mathrm{Cen}$ had a similar
initial mass as its present day mass, then we can place a lower limit on its
time of accretion at t$_{\mathrm{acc}} > 7$ Gyr ago. Alternatively, if the
initial stellar mass was significantly larger, as would be expected if
$\omega\,\mathrm{Cen}$ is the remnant core of a dwarf Galaxy, then we can
constrain the accretion time to t$_{\mathrm{acc}} > 4$ Gyr ago. Taken together,
these results are consistent with the scenario that $\omega\,\mathrm{Cen}$ is
the remnant core of a disrupted dwarf galaxy.
