  Extreme wavefront correction is required for coronagraphs on future space
telescopes to reach 1e-8 or better starlight suppression for the direct imaging
and characterization of exoplanets in reflected light. Thus, a suite of
wavefront sensors working in tandem with active and adaptive optics are used to
achieve stable, nanometer-level wavefront control over long observations. In
order to verify wavefront control systems comprehensive and accurate integrated
models are needed. These should account for any sources of on-orbit error that
may degrade performance past the limit imposed by photon noise. An integrated
model of wavefront sensing and control for a space-based coronagraph was
created using geometrical raytracing and physical optics propagation methods.
Our model concept consists of an active telescope front end in addition to a
charge-6 vector vortex coronagraph instrument. The telescope uses phase
retrieval to guide primary mirror bending modes and secondary mirror position
to control the wavefront error within tens of nanometers. The telescope model
is dependent on raytracing to simulate these active optics corrections for
compensating the wavefront errors caused by misalignments and thermal gradients
in optical components. Entering the coronagraph, a self-coherent camera is used
for focal plane wavefront sensing and digging the dark hole. We utilize
physical optics propagation to model the coronagraph's sensitivity to mid and
high-order wavefront errors caused by optical surface errors and pointing
jitter. We use our integrated models to quantify expected starlight suppression
versus wavefront sensor signal-to-noise ratio.
