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Extreme wavefront correction is required for coronagraphs on future spacetelescopes to reach 1e-8 or better starlight suppression for the direct imagingand characterization of exoplanets in reflected light. Thus, a suite ofwavefront sensors working in tandem with active and adaptive optics are used toachieve stable, nanometer-level wavefront control over long observations. Inorder to verify wavefront control systems comprehensive and accurate integratedmodels are needed. These should account for any sources of on-orbit error thatmay degrade performance past the limit imposed by photon noise. An integratedmodel of wavefront sensing and control for a space-based coronagraph wascreated using geometrical raytracing and physical optics propagation methods.Our model concept consists of an active telescope front end in addition to acharge-6 vector vortex coronagraph instrument. The telescope uses phaseretrieval to guide primary mirror bending modes and secondary mirror positionto control the wavefront error within tens of nanometers. The telescope modelis dependent on raytracing to simulate these active optics corrections forcompensating the wavefront errors caused by misalignments and thermal gradientsin optical components. Entering the coronagraph, a self-coherent camera is usedfor focal plane wavefront sensing and digging the dark hole. We utilizephysical optics propagation to model the coronagraph's sensitivity to mid andhigh-order wavefront errors caused by optical surface errors and pointingjitter. We use our integrated models to quantify expected starlight suppressionversus wavefront sensor signal-to-noise ratio.

Integrated modeling of wavefront sensing and control for space telescopes utilizing active and adaptive optics