  Optimal atmospheric conditions are beneficial for detecting exoplanets via
high contrast imaging (HCI), as speckles from adaptive optics' (AO's) residuals
can make it difficult to identify exoplanets. While AO systems greatly improve
our image quality, having access to real-time estimates of atmospheric
conditions could also help astronomers use their telescope time more
efficiently in the search for exoplanets as well as aid in the data reduction
process. The Shack-Hartmann Imaging Motion Monitor (SHIMM) is an atmospheric
profiler that utilizes a Shack-Hartmann wavefront sensor to create spot images
of a single star in order to reconstruct important atmospheric parameters such
as the Fried parameter ($r_0$), $C_n^2$ profile and coherence time. Due to its
simplicity, the SHIMM can be directly used on a telescope to get in situ
measurements while observing. We present our implementation of the Nickel-SHIMM
design for the one meter Nickel Telescope at Lick Observatory. We utilize an
HCIPy simulation of turbulence propagating across a telescope aperture to
verify the SHIMM data reduction pipeline as we begin on-sky testing. We also
used on-sky data from the AO system on the Shane Telescope to further validate
our analysis, finding that both our simulation and data reduction pipeline are
consistent with previously determined results for the Fried parameter at the
Lick Observatory. Finally, we present first light results from commissioning of
the Nickel-SHIMM.
