Changes between Version 9 and Version 10 of docs/CommissioningPlan/P2.6

Timestamp:

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

Author:

kradhakrishnan

Comment:

--

docs/CommissioningPlan/P2.6

@@ -8 +8 @@
 •       Measure the Non-Common Path Aberrations (NCPA).
 **Prerequisites**
-•       Use of Argos swing arm / RR mounted on the SX side. SHARK-NIR aligned to telescope.
+•       Use of the Argos swing arm / RR mounted on the SX side. SHARK-NIR aligned to telescope.
 * Phase-diversity algorithm is tested and working in simulation and using real-images from the SCICAM (at Padova).
 **Procedure**
 •       Go to a specific elevation of the telescope. 
-* The Arcetri team optimizes the PSF shape on the SCICAM using the trial & error algorithm (used by the LBTO team during LUCI calibrations) changing M2 reference shape applying modes coefficients. [Currently, this is the baseline approach].
-•       For the same elevation, keeping the M2 flat, using the same source, perform the phase-diversity test script which will make use of the Wollaston prism and dual-band imagers 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)].
-•       Make the ALPAO DM flat and using the internal calibration sources, run the phase-diversity script. Apply the obtained NCPA on the ALPAO DM. Take SCICAM images. Note that this NCPA correction does not account for any aberrations caused by the Dichroic and internal TT mirror within the deployable arm. [This NCPA will only be used if the previous two options are not possible or good enough for a given case/target.]
-* Repeat these measurements for decided discreet zenith angles (or elevation of the telescope), SHARK-NIR DROT angle (fixed), and star (source) brightness.
+* 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.
+* 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.
 
 **Success criteria**
-•       NCPA estimated and applied on the ASM.
-•       Satisfactory PSF quality with closed-loop and get a new and improved daytime telescope model for SHARK-NIR?
+•       NCPA estimated and applied on the ALPAO-DM.
+•       Satisfactory PSF quality with closed-loop.
 * The total residual after NCPA correction should be <30nm.
 
@@ -27 +28 @@
 * Authorize SHARK-NIR on the SX side.
 * Permission to use the Argos Swing Arm.
-* When not using Argos swing arm and for different elevation angle tests, RR will be required on the SX side.
+* When not using the Argos swing arm and for different elevation angle tests, RR will be required on the SX side.
 * Support from LBT SW Team