The cumulative effect of the upgrades will be to deliver diffraction-limited imaging and Nyquist-sampled point-spread functions in the , and bands  at nearly double the Strehl ratio of the current system . Nyquist-sampling in all bands is particularly desirable to measure and reconstruct the PSF reliably. The PSF varies because of atmospheric turbulence and the change in gravity vector as the telescope moves - the AO bench is to be mounted at the Cassegrain focus.
The new laser with a pulse format designed to couple better to the Sodium atoms in the upper atmosphere is expected to allow routine use of more subapertures, making better use of the tweeter's spatial frequency sampling ability. Hence, any turbulence will be better measured and corrected because subaperture spacing will be 10 cm for a 3030 lenslet array, which is a much better match to measured conditions at Lick Observatory . In addition, the telescope will be usable over a greater range of the nightly and seasonal variations in mesospheric Sodium levels.
Spectroscopy will also be much improved because of the aforementioned improvements in stability. The ability to reliably rotate the instrument structure and the slit will allow stable object tracking over a longer course of time. Less object wander enables reliable co-adding to raise signal-to-noise ratio (SNR), better tracking of variability in night sky lines and minimizes the impact of hot pixels. The intent of these upgrades is to investigate fainter objects at the diffraction limit of the telescope in all bands and achieve target SNRs in less time. We present the result of modeling the emissivity and throughput of ShaneAO and conservatively predict that the new system will achieve its targets.
Srikar Srinath 2013-10-09