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The Multi Unit Spectroscopic Explorer (MUSE) is an integral fieldspectrograph on the Very Large Telescope Unit Telescope 4, capable of laserguide star assisted and tomographic adaptive optics using the GALACSI module.Its observing capabilities include a wide field (1 square arcmin), ground layerAO mode (WFM-AO) and a narrow field (7.5"x7.5"), laser tomography AO mode(NFM-AO). The latter has had several upgrades in the 4 years sincecommissioning, including an optimisation of the control matrices for the AOsystem and a new sub-electron noise detector for its infra-red low orderwavefront sensor. We set out to quantify the NFM-AO system performance byanalysing $\sim$230 spectrophotometric standard star observations taken overthe last 3 years. To this end we expand upon previous work, designed tofacilitate analysis of the WFM-AO system performance. We briefly describe theframework that will provide a user friendly, semi-automated way for systemperformance monitoring during science operations. We provide the results of ourperformance analysis, chiefly through the measured Strehl ratio and full widthat half maximum (FWHM) of the core of the point spread function (PSF) using twoPSF models, and correlations with atmospheric conditions. These results willfeed into a range of applications, including providing a more accurateprediction of the system performance as implemented in the exposure timecalculator, and the associated optimization of the scientific output for agiven set of limiting atmospheric conditions.

Performance characterization and near-realtime monitoring of MUSE adaptive optics modes at Paranal