Changes between Version 19 and Version 20 of docs/CommissioningPlan/P2.7

Timestamp:

09/23/22 12:54:26 (2 years ago)

Author:

kradhakrishnan

Comment:

--

docs/CommissioningPlan/P2.7

@@ -8 +8 @@
 
 **Description**
-- SHARK-NIR system-level characterization and optimization as a function of the telescope elevation. Checking the pointing offset between SHARK-NIR, LBTI, and SOUL-AO. SOUL-AO tests. Measure the Non-Common Path Aberrations (NCPA).
+- SHARK-NIR system-level characterization and optimization as a function of the telescope elevation. Checking the pointing offset between SHARK-NIR and SOUL-AO. SOUL-AO tests. Measure the Non-Common Path Aberrations (NCPA).
 
 **Prerequisites**
@@ -15 +15 @@
 
 **Procedure for pointing offset measurements and characterization**
-- TBW
+- Check the procedure for the NCPA. This measurements comes as free with the NCPA measurements.
 
 **Procedure for SOUL-AO tests**
-- TBW
+- Check the procedure for the NCPA. This measurements comes as free with the NCPA measurements.
 
 **Procedure for NCPA**
-- Go to a specific elevation of the telescope. 
-- Close the AO loop for the on-axis light source to produce the best PSF at the pin of the pyramid of the SOUL WFS. Keep that shape steady on ASM.
+- Start the tests with telescope pointed to Zenith
+  1. Using the Argos light source / RR light source, acquire the star at the SOUL WFS. 
+  2. Close the AO loop. 
+  3. Check the PSF position at the SCICAM. Move the SOUL WFS stages to position the star the SCICAM center. The stage positions should be same (or very close) to that the values after the alignemnt of SHARK-NIR to the telescope.
+  4. For the AO loop closed that produce the best PSF at the pin of the pyramid of the SOUL WFS, save the ASM shape. Keep that shape steady on ASM.
+  5. Perform the phase diveristy algorithm with flat ALPAO DM. The focus is introduced by the ASM bymoving the LGS WFS in focal direction. 
+  6. Ideally, contrast is the metric to be used to find the best NCPA shape for the ALPAO DM. However, since the contrast is directly related to the PSF optical quality at the coronagraphic focal plane which is the same (or very close to same) at the scientific focal plane, we will use the SCICAM PSF images to determine the aberrations and therefore to find the best shape to apply on the ALPAO DM.
+  7. Only for Zenith angle, the following tests are also performed:
+
+
+- 
 - Now, optimize the PSF shape on the SCICAM using the trial & error algorithm. The ALPAO-DM on the SHARK-NIR Bench is used to apply different modes. [Currently, this is the baseline approach].
 - For the same elevation, keeping the same ASM shape as before and the same source, perform the phase-diversity test (with flat ALPAO-DM), using the Wollaston prism and dual-band imager lens configuration. Apply the obtained NCPA on the ALPAO DM within SHARK. Take SCICAM images to see the improvement. [In case the NCPA produced by the baseline approach is not stable enough for a longer period, and if more correction seems necessary for high contrast, we will be implementing this approach (for which we will be using the star itself as the source during nighttime)].
@@ -28 +37 @@
 - Repeat these measurements for the decided discreet zenith angles (or elevation of the telescope) and SHARK-NIR DROT angle (fixed).
 
+
+after ncpa_ zenith soul close loop on an aberrated PSF 
 
 **Templates**