Changes between Version 7 and Version 8 of docs/CommissioningPlan/P3.8

Timestamp:

04/22/22 20:48:37 (3 years ago)

Author:

kradhakrishnan

Comment:

--

docs/CommissioningPlan/P3.8

@@ -1 @@
-== P3.8 Internal TT loop working and performance== 
+== P3.8 NCPA working and performance & checking for pupil shifts == 
  
 - **Phase**             :       3  
@@ -5 +5 @@
 - **Category**  :       Nighttime testing (functionality and operability) (C5) + Nighttime testing for performance (C7)
 - **Recurrence**        :       once at commissioning
-- **Duration**  :       1 night
+- **Duration**  :       8 hours
 
 **Description**
-- Evaluate the performance of the internal tip-tilt (TT) loop of SHARK-NIR for stars of varying brightness.
+- Evaluate the NCPA working and performance using the baseline approach, phase-diversity approach using the Wollaston prism & dual-band imaging, and measurement of NCPA using SHARK-NIR internal calibration sources.
 
 **Prerequisites**
 - Atmospheric conditions: TBD
 - Authorize SHARK-NIR on the SX side.
-- Stars (of known brightness from 8mag-13mag in R band) as targets.
 - AO is working.
+- Target(s) at different Zenith distances with different magnitudes.
+- lookup tables of already calibrated NCPA measurements.
 
 **Procedure**
-- Run the internal TT loop after the star is acquired and the AO loop is closed. 
-- Take unsaturated images of the star for a given (?) science filter before and after the internal TT loop closure in the SCICAM.
-- Take data in TECCAM simultaneously. 
-- Use data to estimate the improvement of the residual jitter after the TT loop is closed.
-- Repeat for different star magnitudes.
-- should we perform as a function of elevation as well? We can choose stars accordingly, then?
+- Acquire a star of a given magnitude, start SOUL-AO, followed by the internal-TT loop.
+- Check the working and performance of the NCPA (already calibrated) baseline approach. Take images at SCICAM.
+- Check the phase diversity NCPA approach using Wollaston prism + DI-DBI (already calibrated). Take images at SCICAM.
+- If the PSF after applying the calibrated NCPA is bad, we could close the SHARK-NIR shutter (can have the SOUL-AO running parallel) and do a quick internal NCPA measurement (either till the NCPA modal coefficients or until the new shape on ALPAO-DM) to confirm that the alignment of SHARK-NIR is still good. This would mean that the NCPA already calibrated is not good enough!
+- Measure the phase diversity NCPA approach using Wollaston prism + DI-DBI  and using real star (need to do on the spot, but script exists). Take images at SCICAM.
+- Check the pupil position by inserting the pupil lens.
+- Repeat for a different star (of various magnitudes and for a different telescope elevation). It is also good to do this for other seeing conditions.
 
 **Templates**
-- SHARKNIR_gen_tiptilt_loop (not released)
+- SHARKNIR_di_cal_NCPA (not released)
 
 **Success criteria**
-- Estimate the residual jitter after SOUL-AO is closed for a given seeing and star brightness.
-- Checking the working and performance of the internal TT loop.
-- Quantify and numbers to add?
+- NCPA estimated and applied on the ASM / ALPAO DM.
+- Cross-check the NCPA performances with the daytime activity [wiki:/docs/CommissioningPlan/P2.6 P2.6].
+- The total residual after NCPA correction should be <30nm.
 
 **Notes**
@@ -38 +40 @@
 
 **Date performed and by whom**
+
+**comment**
+- perform for 5 cases e.g. Rmag 8, 10, 10, 12, 14. These five cases where the star has different mag and at different zenith angles over different nights (so different seeing).