Changes between Version 6 and Version 7 of docs/CommissioningPlan/P4.3

Timestamp:

02/04/21 14:58:11 (4 years ago)

Author:

kradhakrishnan

Comment:

--

docs/CommissioningPlan/P4.3

@@ -1 @@
-== 4.3 Exo-planet: Spectroscopic Characterization of known sub-stellar companions        == 
+== 4.3 Disk: High-contrast images of circumstellar disks         == 
 •       **Phase**               :       4  
 •       **Status**              :       Draft    
 •       **Category**            :       Science verification / Early science (C8)
 •       **Recurrence**  :       once after the completion of nighttime testing and performance check
-•       **Duration**            :       5 night(s)
+•       **Duration**            :       4 night(s)
 **Description**
-•       Exo-planet: Spectroscopic Characetization of known sub-stellar companions
+•       Disk: High-contrast images of circumstellar disks
 **Prerequisites**
 •       Authorize SHARK-NIR on the SX side.
 •       Atmospheric conditions: CLEAR
 •       Bad pixel map, Background or Dark, Flat-field, distortion map 
-•       Cloud Cover             : no clouds
+•       Cloud Cover             : no cloud
 •       Astronomical Seeing     : 0.8" or better
 •       Sky Background  : Any
 •       Water Vapor             : low
-•       Timing Windows  : no need to observe during meridian passage (field stabilized observing mode)
-•       Observing Targets       : TBD We will consider stars with H mag in the range 4-12 (typical 7-9), R will have a similar distribution. Targets with a known companion at separation larger than 0.4" from the star and with contrast larger than 1E-5).
-•       Observing Filters       : LSS observing mode, no filter
-•       Detector Mode, DIT: according to the brightness of the target
-•       Daytime Calibration Data required: dark/background, flat, wavelength calibration
-•       Nighttime Calibration Data required: none
+•       Timing Windows  : better to observe during the passage of the target at the meridian (+/- 1 hour before)
+•       Observing Targets       : TBD. We will consider stars with H mag in the range 4-12 (typical 7-9), R will have a similar distribution. It would be better to observe target with disk yet observed in NIR)
+•       Observing Filters       : TBD
+•       Detector Mode, DIT: according to the target brightness
+•       Daytime Calibration Data required: dark/background, flat
+•       Nighttime Calibration Data required: flux calibration, star centering
 
 **Procedure**
-•       We observe for more than 1 hour the star with the LSS observing mode. 
-* We alternate the position of the slits from the position of the companion to outside the companion position to be able to create a library of images to be used to subtract the speckles. 
-* An observation of the star without the coronagraphic mask is also requested to allow a proper flux calibration. 
-* Also, we need observation of a standard star to be able to properly reduce the telluric lines. 
-* The observation is performed in field stabilized mode. 
+•       After pre-set and acquisition of the target we will run on 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. 
+* 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 the ADI. This part should be at least 1:20-1:30 hours long. 
+* The observation is closed running again the centering and flux calibration templates with the same modalities adopted at the beginning of the observations.
+
 **Notes**