  Exoplanet detection and characterization through extreme adaptive optics
(ExAO) is a key science goal of future extremely large telescopes. This
achievement, however, will be limited in sensitivity by both quasi-static
wavefront errors and residual AO-corrected atmospheric wavefront errors. A
solution to both of these problems is to use the science camera of an ExAO
system as a wavefront sensor to perform a fast measurement and correction
method to remove these aberrations as soon as they are detected. We have
developed the framework for one such method, using the self-coherent camera
(SCC), to be applied to ground-based telescopes, called Fast Atmospheric SCC
Technique (FAST; Gerard et al., submitted). Our FAST solution requires an
optimally designed coronagraph (the SCC FPM) and post-processing algorithm and
is in principle able to reach a "raw" contrast of a few times the photon noise
limit, continually improving with integration time. In this paper, we present
new ongoing work in exploring the manufacturing limitations of the SCC FPM as
well as a general framework to implement and optimize a FAST deformable mirror
control loop.
