  Pupil mapping is a promising and unconventional new method for high contrast
imaging being considered for terrestrial exoplanet searches. It employs two (or
more) specially designed aspheric mirrors to create a high-contrast amplitude
profile across the telescope pupil that does not appreciably attenuate
amplitude. As such, it reaps significant benefits in light collecting
efficiency and inner working angle, both critical parameters for terrestrial
planet detection. While much has been published on various aspects of pupil
mapping systems, the problem of sensitivity to wavefront aberrations remains an
open question. In this paper, we present an efficient method for computing the
sensitivity of a pupil mapped system to Zernike aberrations. We then use this
method to study the sensitivity of a particular pupil mapping system and
compare it to the concentric-ring shaped pupil coronagraph. In particular, we
quantify how contrast and inner working angle degrade with increasing Zernike
order and rms amplitude. These results have obvious ramifications for the
stability requirements and overall design of a planet-finding observatory.
