Changes between Version 10 and Version 11 of docs/CommissioningPlan/P4.6


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Timestamp:
02/04/21 15:19:09 (4 years ago)
Author:
kradhakrishnan
Comment:

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  • docs/CommissioningPlan/P4.6

    v10 v11  
    1 == 4.6 Exo-planet: Giant planets and brown dwarfs in SFR, stellar associations, & young open clusters    ==
     1== 4.6 Disk: Jets investigated with long-slit spectra    ==
    22•       **Phase**               :       4 
    33•       **Status**              :       Draft   
    44•       **Category**            :       Science verification / Early science (C8)
    55•       **Recurrence**  :       once after the completion of nighttime testing and performance check
    6 •       **Duration**            :       10 night(s)
     6•       **Duration**            :       1 night(s)
    77**Description**
    8 •       Exo-planet: Giant planets and brown dwarfs in SFR, stellar associations, & young open clusters
     8•       Disk: Jets investigated with long-slit spectra
    99**Prerequisites**
    1010•       Authorize SHARK-NIR on the SX side.
    … …  
    1515•       Sky Background  : Any
    1616•       Water Vapor             : low
    17 •       Timing Windows  : better to observe during the passage of the target at the meridian (+/- 1 hour before)
    18 •       Observing Targets       : TBD. We will consider stars with H mag in the range 4-12 (typical 7-9), R will have a similar distribution.
    19 •       Observing Filters       : TBD
    20 •       Detector Mode, DIT: according to the target brightness (TBD)
    21 •       Daytime Calibration Data required: dark/background, instrument flat
    22 •       Nighttime Calibration Data required: flux calibration and centering data (only in case of coronagraphic observation - standard case)
     17•       Timing Windows  : no major limitation as the observation will be done in filed stabilized mode
     18•       Observing Targets       : TBD (same than in Section 4.10)
     19•       Observing Filters       : LSS observing mode, no filter
     20•       Detector Mode, DIT: according to the target brightness
     21•       Daytime Calibration Data required: dark/background, flat
     22•       Nighttime Calibration Data required: none
    2323
    2424**Procedure**
    25 •       After pre-set and acquisition of the target, we will run a flux calibration template with the star off-centered from the coronagraph (short template - few minutes). After this, a centering observation follows with the Fourier mode on the DM allowing the creation of four satellite spots (around 5% of the target brightness). Also, this template is short.
    26 * We then perform the scientific coronagraphic observation using pupil stabilized observing mode. This observation should be taken during the passage of the star to the meridian to maximize the rotation of the FOV and allowing to implement ADI. This part should be at least 1:20-1:30 hours long. 
    27 * At the end of the observation, the centering and flux calibration templates are executed with the same modalities adopted at the beginning of the observations.
     25•       We observe for more than 1 hour the star with the LSS observing mode.
     26* We alternate the position of the slits from the position of the jet to outside the companion position to be able to create a library of images to be used to subtract the speckles.
     27* An observation of the star without a coronagraphic mask is also requested to allow a proper flux calibration.
     28* Also, we need observation of a standard star to properly reduce the telluric lines.
     29* The observation is performed in field stabilized mode.
    2830**Notes**
    2931