  We build on previous efforts to model CCD sensors, during illumination and
collection of conversions. We use a finite summation of simple, electrostatic
field models. The upgraded functionality of our framework provides specific
predictions for perturbations in pixel boundary enclosures (e.g., at the
backside window) and the bookkeeping capability to stack those perturbations so
that they may be utilized as Greens functions -- portable calculation results
that may be generically applied to a range of precision astronomy related
problems that naturally including astrometric, photometric and shape transfer
issues. We approach the topic of using ancillary pixel data, derived from the
Greens function and the registered image, to analyze sky data and constrain
object parameters of astronomical targets.
