Changes between Version 14 and Version 15 of docs/CommissioningPlan/P2.6


Ignore:
Timestamp:
01/14/22 15:36:40 (3 years ago)
Author:
kradhakrishnan
Comment:

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  • docs/CommissioningPlan/P2.6

    v14 v15  
    1 == P2.6 Measurement of NCPA ==
    2 •       **Phase**               :       2 
    3 •       **Status**              :       Draft   
    4 •       **Category**            :       Daytime testing (functionality and operability) (C3) + Daytime calibration (C4)
    5 •       **Recurrence**  :       after instrument installation at telescope platform
    6 •       **Duration**            :       8 days
     1== P2.6 NCPA measurements ==
     2
     3- **Phase**             :       2 
     4- **Status**            :       Draft   
     5- **Category**  :       Daytime testing (functionality and operability) (C3) + Daytime calibration (C4)
     6- **Recurrence**        :       once after instrument installation at telescope platform
     7- **Duration**  :       8 days
     8
    79**Description**
    8 •       Measure the Non-Common Path Aberrations (NCPA).
     10- Measure the Non-Common Path Aberrations (NCPA).
     11
    912**Prerequisites**
    10 •       Use of the Argos swing arm / RR mounted on the SX side. SHARK-NIR aligned to telescope.
    11 * Phase-diversity algorithm is tested and working in simulation and using real-images from the SCICAM (at Padova).
     13- Use the Argos swing arm / RR mounted on the SX side. SHARK-NIR aligned to telescope.
     14- Phase-diversity algorithm is tested and working in simulation and using real-images from the SCICAM (at Padova).
     15
    1216**Procedure**
    13 •       Go to a specific elevation of the telescope.
    14 * 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.
    15 * 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].
    16 •       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)].
    17 •       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.
    18 * Repeat these measurements for the decided discreet zenith angles (or elevation of the telescope) and SHARK-NIR DROT angle (fixed).
     17- Go to a specific elevation of the telescope.
     18- 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.
     19- 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].
     20- 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)].
     21- 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.
     22- Repeat these measurements for the decided discreet zenith angles (or elevation of the telescope) and SHARK-NIR DROT angle (fixed).
     23
     24**Templates**
    1925
    2026**Success criteria**
    21 •       NCPA estimated and applied on the ALPAO-DM.
    22 •       Satisfactory PSF quality with closed-loop.
    23 * The total residual after NCPA correction should be <30nm.
     27- NCPA estimated and applied on the ALPAO-DM.
     28- Satisfactory PSF quality with closed-loop.
     29- The total residual after NCPA correction should be <30nm.
    2430
    2531**Notes**
    26 •       See activity 8.1 in AD4 for more details.
     32- See activity 8.1 in AD4 for more details.
     33
    2734**LBTO support**
    28 * Authorize SHARK-NIR on the SX side.
    29 * Permission to use the Argos Swing Arm.
    30 * When not using the Argos swing arm and for different elevation angle tests, RR will be required on the SX side.
    31 * AO support.
    32 
    33 
    34 **Associated SHARK-NIR personnel**
    35 
     35- Authorize SHARK-NIR on the SX side.
     36- Permission to use the Argos Swing Arm.
     37- RR will be required on the SX side when not using the Argos swing arm and for different elevation angle tests.
     38- AO support.
    3639
    3740**Date performed and by whom**
    3841
    3942**Comments**
    40 * add dynamic disturbance at ASM for 0.7", 1", 1.5" - looks t open loop and closed loop strehl. then closed loop + TT strehl, then closed loop + TT + NCPA corrected strehl.
     43- add dynamic disturbance at ASM for 0.7", 1", 1.5" - looks t open loop and closed loop strehl. then closed loop + TT strehl, then closed loop + TT + NCPA corrected strehl.