Changes between Version 11 and Version 12 of docs/CommissioningPlan/P2.6

Timestamp:

02/05/21 17:12:04 (4 years ago)

Author:

kradhakrishnan

Comment:

--

docs/CommissioningPlan/P2.6

@@ -12 +12 @@
 **Procedure**
 •       Go to a specific elevation of the telescope. 
-* Close the AO loop to produce the best PSF at the pin of the pyramid of the SOUL WFS. KEep that shape steady on ASM.
+* 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.
 * 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) making use of 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/or 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)].
 •       Note that in the above two cases, the optical path contains the same optics (except for the Wollaston and DBI lens) including the dichroic and IN_TT of the deployable arm. 
-* Repeat these measurements for the decided discreet zenith angles (or elevation of the telescope), SHARK-NIR DROT angle (fixed), and star (source) brightness.
+* Repeat these measurements for the decided discreet zenith angles (or elevation of the telescope) and SHARK-NIR DROT angle (fixed).
 
 **Success criteria**