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Optimal atmospheric conditions are beneficial for detecting exoplanets viahigh contrast imaging (HCI), as speckles from adaptive optics' (AO's) residualscan make it difficult to identify exoplanets. While AO systems greatly improveour image quality, having access to real-time estimates of atmosphericconditions could also help astronomers use their telescope time moreefficiently in the search for exoplanets as well as aid in the data reductionprocess. The Shack-Hartmann Imaging Motion Monitor (SHIMM) is an atmosphericprofiler that utilizes a Shack-Hartmann wavefront sensor to create spot imagesof a single star in order to reconstruct important atmospheric parameters suchas the Fried parameter ($r_0$), $C_n^2$ profile and coherence time. Due to itssimplicity, the SHIMM can be directly used on a telescope to get in situmeasurements while observing. We present our implementation of the Nickel-SHIMMdesign for the one meter Nickel Telescope at Lick Observatory. We utilize anHCIPy simulation of turbulence propagating across a telescope aperture toverify the SHIMM data reduction pipeline as we begin on-sky testing. We alsoused on-sky data from the AO system on the Shane Telescope to further validateour analysis, finding that both our simulation and data reduction pipeline areconsistent with previously determined results for the Fried parameter at theLick Observatory. Finally, we present first light results from commissioning ofthe Nickel-SHIMM.

SHIMM as an atmospheric profiler on the Nickel Telescope