Changes between Version 1 and Version 2 of docs/CommissioningPlan/P3.22


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Timestamp:
02/04/21 14:50:06 (4 years ago)
Author:
kradhakrishnan
Comment:

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  • docs/CommissioningPlan/P3.22

    v1 v2  
    1  == P3.22       Instrument flat field, detector linearity and bad pixels ==
    2 •       **Phase**               :       3 
     1== 3.22 Coronagraphic imaging + field stabilization mode testing        ==
     2•       **Phase**               :       4 
    33•       **Status**              :       Draft   
    4 •       **Category**            :       Daytime calibration (C3)
    5 •       **Recurrence**  :       every day, with setup on request.
    6 •       **Duration**            :       20 minutes per configuration
     4•       **Category**            :       Nighttime testing for functionality, operability, and performance (C5 + C7)
     5•       **Recurrence**  :       once
     6•       **Duration**            :       1 night(s)
    77**Description**
    8 •       Instrument flat field, detector linearity, and bad pixels.
     8•       Dedicated to check the complete procedure and running of the OB scripts through SHINS for all the combinations of this observing mode.
    99**Prerequisites**
     10•       Authorize SHARK-NIR on the SX side.
     11•       Atmospheric conditions: ?
     12•       Atmospheric conditions: ?
     13•       Bad pixel map, Background or Dark, Flat-field, distortion map
     14•       Cloud Cover             :
     15•       Astronomical Seeing     :
     16•       Sky Background  : Any / Bright
     17•       Water Vapor             : Any
     18•       Timing Windows  :
     19•       Observing Targets       :
     20•       Observing Filters       :
     21•       Detector Mode, DIT:
     22•       Daytime Calibration Data required:
     23•       Nighttime Calibration Data required:
     24
    1025**Procedure**
    11 •       Use the calibration flat-field source.
    12 •       This calibration is performed illuminating the detector uniformly using the instrument FF lamp, for each filter.
    13 •       It is expected that the detector FF depends on filters, final accumulated charge in the pixels. Thus, a series of exposures will be taken at different count levels (realized via ND filters and/or DIT) for each filter setup. In this case, the template takes the background frames automatically. Comparing different count rates at constant DIT will also yield a linearity map of the detector.
    14 **Success criteria**
    15 •       95% luminous uniformity at large scale.
    16 •       99% luminous uniformity at pixel-to-pixel scale 10-2.
    17 •       Large scales filtered out, only small detector scale will remain. Effect of the large-scale flat field on DBI (rescaling in flux & wavelength) has negligible impact on DBI performances.
     26•       ?
    1827**Notes**
    19 •       Same as activity 7.9 in AD4
     28
    2029**LBTO support**
    21 •       Support from LBTI/LBTO?
     30•       SOUL-AO support
     31
    2232**Associated SHARK-NIR personnel**
    23 •       JF, LM, MdP
     33
     34       
    2435**Date performed and by whom**