Simulating Eclipsing Binary Yields of the Rubin Observatory in the
  Galactic Field and Star Clusters
  We present a study of the detection and recovery efficiency of the Rubin
Observatory for detached eclipsing binaries (EBs) in the galactic field,
globular clusters (GCs) and open clusters (OCs), with a focus on comparing two
proposed observing strategies: a standard cadence ("baseline"), and a cadence
which samples the galactic plane more evenly ("colossus"). We generate
realistic input binary populations in all observing fields of the Rubin
Observatory, simulate the expected observations in each filter, and attempt to
characterize the EBs using these simulated observations. In our models, we
predict the baseline cadence will enable the Rubin Observatory to observe about
three million EBs; our technique could recover and characterize nearly one
million of these in the field and thousands within star clusters. If the
colossus cadence is used, the number of recovered EBs would increase by an
overall factor of about 1.7 in the field and in globular clusters, and a factor
of about three in open clusters. Including semi-detached and contact systems
could increase the number of recovered EBs by an additional factor of about 2.5
to 3. Regardless of the cadence, observations from the Rubin Observatory could
reveal statistically significant physical distinctions between the
distributions of EB orbital elements between the field, GCs and OCs.
Simulations such as these can be used to bias correct the sample of Rubin
Observatory EBs to study the intrinsic properties of the full binary
populations in the field and star clusters.
