  The ambitious goals of precision cosmology with wide-field optical surveys
such as the Dark Energy Survey (DES) and the Large Synoptic Survey Telescope
(LSST) demand, as their foundation, precision CCD astronomy. This in turn
requires an understanding of previously uncharacterized sources of systematic
error in CCD sensors, many of which manifest themselves as static effective
variations in pixel area. Such variation renders a critical assumption behind
the traditional procedure of flat fielding--that a sensor's pixels comprise a
uniform grid--invalid. In this work, we present a method to infer a curl-free
model of a sensor's underlying pixel grid from flat field images, incorporating
the superposition of all electrostatic sensor effects--both known and
unknown--present in flat field data. We use these pixel grid models to estimate
the overall impact of sensor systematics on photometry, astrometry, and PSF
shape measurements in a representative sensor from the Dark Energy Camera
(DECam) and a prototype LSST sensor. Applying the method to DECam data recovers
known significant sensor effects for which corrections are currently being
developed within DES. For an LSST prototype CCD with pixel-response
non-uniformity (PRNU) of 0.4%, we find the impact of "improper" flat-fielding
on these observables is negligible in nominal .7" seeing conditions. These
errors scale linearly with the PRNU, so for future LSST production sensors,
which may have larger PRNU, our method provides a way to assess whether
pixel-level calibration beyond flat fielding will be required.
