This section presents the expected imaging sensitivities for GSAOI. The first table lists the limiting magnitude, the saturation magnitude, the assumed Strehl ratio and the sky brightness for each filter. The second table lists the background contribution from different sources for all filters. The imaging sensitivities presented here are theoretical and have been obtained using a model for the object (point-source) and background signals. These estimated values are a good approximation of what it is expected for GSAOI. Accurate sensitivity values will be derived during the GSAOI and GeMS commissioning. For the modeling, the following parameters were assumed:

• Detector dark current of 0.05 e-/s/pix, a read noise of 5 e-, using multiple reads and detector quantum efficiency of ~ 80%
• Background signal considerations: airglow emission and thermal emission from the sky, telescope, cryostat window, cryostat interior and GeMS.
  
  

(1) Saturation magnitudes are estimated assuming a minimum integration time of 5 sec and detector full well depth of 50,000e-

(*)  Model background signals for each filter assume a dark current of 30 e-/s/pix in 600 sec integration.

Note: the model background signals for each filter presented in the table have to be verified and confirmed during the GeMS + GSAOI commissioning.