README web version of /home/usg/OPS/MTS/readme_xml/readme_82503700

Principal Investigator Email Address

• lagrange@obs.ujf-grenoble.fr

Estimated Total Execution Time (hours, including overheads)

• 1h44

General Description

• Our aim is to reproduce the conditions that lead us to image a possible
   planet companion to beta Pictoris in nov 2003 Naco data.
  
  To do so, we need to record saturated images of beta Pictoris (herefater bpic) and
   saturated images of a PSF star (also called comparison star, as in the proposal)
   (hr2435). We will also record unsaturated images of both stars (which will be used
   as PSF and photometric references).
   
  Each OB consists of:
  	- an acquisition template
  	- a science template to get unsaturated images (using the NDL filter) at different
   generic offsets 
  	- 2 or 3 science templates to get saturated images, at different generic offsets
  
  There are time-critical/execution constraints associated to these observations:
  1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
   the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
   ie at LST in the range 04h17--05h17.
  
  2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
   Bpic OB should be executed in 44 minutes precisely. In order to take into account
   the uncertainty in the duration of the acquisition process, the OBs as prepared
   last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
   to STOP the OB 44 minutes after starting beta Pic pointing and proceed immediately
   with the PSF OB. It is imperative that the PSF proceed without any delay after Bpic.
   The PSF OB should last 44 minutes as well.
  
  3- Please avoid any delay between acquisitionas and science frames.
  
  Important notes:
  - finding charts: in both cases, the brightest object will be the targets themselves;
   hence for bpic_Lp_runA, L' = 3.5 and for the PSF_bpic_Lp_runA, the brightest object
   has L' ~ 4.
  - in all cases, the offset patterns assume that the targets are centered in the
   FoV at the beginning of the template (ie prior to the first offset)
  - the DITs of the unsaturated images (using the NDL filter) have been calculated
   using the ETC; they are supposed to avoid the non linearity domain. If the level
   of non linearity is reached at acquisition, please adjust the DIT so as to avoid
   this non linearity domain.
  - the DITs of the saturated images of bpic have been defined to saturate the core
   of the PSF over a radius of 4 to 5 pixels. Please adjust the DIT according to the
   actual observing conditions at the beginning of each template.
  - same for the PSF.
  - we have assumed (Naco UM, p 27) that twighlight flats would be done as part of
   Naco Calibration plan.
  - we made a waiver request to observe the two targets which are brighter than L'=5
   and one to ask to execute the PSF OB immediately after the science OB.
  - both targets will be used as a reference for AO
  - both targets are the only bright objects in the conica FoV

Waiver Requests

• Waiver requests have been sent :
  - to ask to be allowed to observe beta pic and hr2435 whch are brighter than 5 at
   L'.
  - to ask to execute the PSF OB immediately after the OB of the science target, bpic.
  - to ask to prepare OBs with durations longer than what we need (see REDAME file)

Critical Observing Condition Constraints

• AM < 1.2
  seeing < 0.8. the image quality is really mandatory for us.

Time-Critical Aspects

• There are timing constraints associated to these observations:
  1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
   the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
   ie at LST in the range 04h17--05h17.
  
  2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
   Bpic OB should be executed in 44 minutes precisely. In order to take into account
   the uncertainty in the duration of the acquisition process, the OBs as prepared
   last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
   to STOP the OB 44 minutes after starting beta Pic pointing and proceed immediately
   with the PSF OB. It is imperative that the PSF proceed without any delay after Bpic.
   The PSH OB should last 44 minutes as well.
  
  3- Please avoid any delay between acquisitionas and science frames.

Special Execution Requirements

• There are timing constraints associated to these observations:
  1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
   the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
   ie at LST in the range 04h17--05h17.
  
  2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
   Bpic OB should be executed in 44 minutes precisely. In order to take into account
   the uncertainty in the duration of the acquisition process, the OBs as prepared
   last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
   to STOP the OB 44 minutes after starting beta Pic pointing and proceed immediately
   with the PSF OB. It is imperative that the PSF proceed without any delay after Bpic.
   The PSH OB should last 44 minutes as well.
  
  3- Please avoid any delay between acquisitionas and science frames.

Special Calibration Information

• NA

ToO Information

• NA

ToO Activators List

• NA

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• NA

Source(s) of Pre-imaging

• ---(Empty)---

Pre-imaging sources not listed above

• ---(Empty)---

Do all your OBs comply with the instrument-specific requirements listed
 on the instrument-specific Phase 2 web page ?

• YES

If this is a pre-imaging run, did you select PRE-IMAGING for the Observing
 Category for each Observing Template ?

• N/A

Do all your finding charts comply with both the general and instrument-specific
 Phase 2 Web Pages ?

• YES

If you submitted OBs for standard stars, did you specify the magnitude
 and spectral type of all standard stars in the OBs ?

• N/A

Have you included OBs for any calibrations that you need but which are
 not part of the Calibration Plan ?

• N/A

If you are observing Moving Targets, have you attached suitable ephemeris
 files to your OBs?

• N/A

If you have preferences which OBs should be executed first, did you make
 use of the User Priority field in the OBs ?

• YES

If this is a run that requires coordinated observations with other facilities,
 did you give proper instructions in the Time-Critical Aspects Section ?

• N/A

If you have PSF reference star OBs, do the names of those OBs begin with
 PSF_ ?

• YES

If there are Finding Charts attached to your OBs, is the field-of-view
 of at least one of these charts 2' x 2' (with clearly labelled field orientation)
 ?

• YES

Have you clearly marked and labelled your wavefront reference objects
 R1, R2, R3, ... (as specified in the NAOS Preparation Software) on your Finding
 Charts ?

• YES

Have you specified the magnitude of the brightest object in the field-of-view
 for each OB ?

• YES

Are there objects in any of your fields (including standard stars) which
 are brighter than the limits specified in the User Manual and on NACO web Pages
 ?

• YES

If the previous answer is yes, have you given a list of OBs and a justification
 for the brightness limit violation in the general description field ?

• YES