  Millisecond focal plane telemetry is now becoming practical due to a new
generation of near-IR detector arrays with sub-electron noise that are capable
of kHz readout rates. Combining these data with those simultaneously available
from the wavefront sensing system allows the possibility of self-consistently
determining the optical aberrations (the cause of quasi-static speckles) and
the planetary image. This approach may be especially advantageous for finding
planets within about 3 $\lambda / D$ of the star where differential imaging is
ineffective. As shown in a recent article by the author (J. Opt. Soc. Am. A.,
33, 712, 2016), one must account for unknown aberrations in several
non-conjugate planes of the optical system, which, in turn, requires ability to
computational propagate the field between these planes. These computations are
likely to be difficult to implement and expensive. Here, a far more convenient
alternative based on empirical Green's functions is provided. It is shown that
the empirical Green's function (EGF), which accounts for all multi-planar,
non-common path aberrations, and results in a much more tractable and highly
parallel computational problem. It is also shown that the EGF can be
generalized to treat polarization, resulting in the empirical Green's tensor
(EGT).
