  Gravitational wave detectors are observing compact object mergers from
increasingly far distances, revealing the redshift evolution of the binary
black hole (BBH) -- and soon the black hole-neutron star (BHNS) and binary
neutron star (BNS) -- merger rate. To help interpret these observations, we
investigate the expected redshift evolution of the compact object merger rate
from the isolated binary evolution channel. We present a publicly available
catalog of compact object mergers and their accompanying cosmological merger
rates from population synthesis simulations conducted with the COMPAS software.
To explore the impact of uncertainties in stellar and binary evolution, our
simulations use two-parameter grids of binary evolution models that vary the
common-envelope efficiency with mass transfer accretion efficiency, and
supernova remnant mass prescription with supernova natal kick velocity,
respectively. We quantify the redshift evolution of our simulated merger rates
using the local ($z\sim 0$) rate, the redshift at which the merger rate peaks,
and the normalized differential rates (as a proxy for slope). We find that
although the local rates span a range of $\sim 10^3$ across our model
variations, their redshift-evolutions are remarkably similar for BBHs, BHNSs,
and BNSs, with differentials typically within a factor $3$ and peaks of
$z\approx 1.2-2.4$ across models. Furthermore, several trends in our simulated
rates are correlated with the model parameters we explore. We conclude that
future observations of the redshift evolution of the compact object merger rate
can help constrain binary models for stellar evolution and gravitational-wave
formation channels.
