  The Nancy Grace Roman Space Telescope (Roman) mission is expected to launch
in the mid-2020s. Its weak lensing program is designed to enable unprecedented
systematics control in photometric measurements, including shear recovery,
point-spread function (PSF) correction, and photometric calibration. This will
enable exquisite weak lensing science and allow us to adjust to and reliably
contribute to the cosmological landscape after the initial years of
observations from other concurrent Stage IV dark energy experiments. This
potential requires equally careful planning and requirements validation as the
mission prepares to enter its construction phase. We present a suite of image
simulations based on GalSim that are used to construct a complex, synthetic
Roman weak lensing survey that incorporates realistic input galaxies and stars,
relevant detector non-idealities, and the current reference five-year Roman
survey strategy. We present a first study to empirically validate the existing
Roman weak lensing requirements flowdown using a suite of 12 matched image
simulations, each representing a different perturbation to the wavefront or
image motion model. These are chosen to induce a range of potential static and
low- and high-frequency time-dependent PSF model errors. We analyze the
measured shapes of galaxies from each of these simulations and compare them to
a reference, fiducial simulation to infer the response of the shape measurement
to each of these modes in the wavefront model. We then compare this to existing
analytic flowdown requirements, and find general agreement between the
empirically derived response and that predicted by the analytic model.
