Expected performance of the Pyramid wavefront sensor with a laser guide star for 40 m class telescopes

Open Access

Fig. 14

Strehl ratio for E2E simulations (markers) and sensitivity predictions (solid lines) of closed-loop performance for 8 (top plot) and 16 m (bottom plot) telescopes. $σ_{noise}^{2}$ $\[\sigma_{\text {noise }}^2\]$ corresponds to the residual variance predicted by fitting error and photon noise for NGS, LGS-2D, and LGS-3D. The yellow stripe corresponds to the expected return flux of the LGSs for the ELT.

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