README web version of /home/usg/OPS/MTS/readme_xml/readme_79080400

Principal Investigator Email Address

• fpatat@eso.org

Estimated Total Execution Time (hours, including overheads)

• 06:03:46

General Description

• This is a simple LSS programme on a faint (V~21) Supernova of type Ia,
   aimed at covering one single epoch at about one year after the explosion.
  
  It includes 6 OBs subdivided into LSS (5 OBs) and BV imaging (1 OB). 
  
  The exact brightness of the target is not known, but it is expected to be around
   V=21. The finding charts provided with the OBs have been produced using archival
   FORS1 images on which an artificial star with the suitable magnitude and at the
   precise SN positions has been added.
  While the position is accurate to within 0.1 arcsec, the actual brightness of the
   SN might be different from what is reported by the finding charts.
  
  Note that we have supplied two f.charts, one with a 4'x4' field-of-view and a 40"x40"
   zoom,
  where the target and the neigboring objects are clearly visible.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• No critical observing conditions constraints.

Time-Critical Aspects

• We would like to obtain all observations within 7-10 days. Best observability
   is April/May.

Special Execution Requirements

• If possible, once the programme is started, it should be completed within
   7-10 days.
  If the OBs are executed in pairs, the program will be completed in 3 separated nights.
  
  Ideally, the imaging OB should be executed just after or just before one of the
   LSS OBs.
  We are aware that, due to operational issues, this might not be the case.

Special Calibration Information

• Science observations are done with the 300V grisms without Order Sorting
   filter, since the flux in the blue end of the spectrum is very low and hence we
   do not expect any measurable second order contamination above 6500A. 
  
  As foreseen by the Calibration Plan, the specphot standard stars will be observed
   with the same setup. This can be a problem if the specphot star is very blue, as
   it often happens. This would of course turn into a wrong sensitivity function and
   hence into a wrong flux calibration of
  our science data.
  
  For this reason, we kindly ask the night astronomers to observe the specphot standard
   star
  without the Order Sorting filter (as foreseen by the Calibration Plan) and to repeat
   the
  exposure WITH GG435 each time this is possible and does not interfere with normal
   operations.
  
  We will then combine both observations (with and without OS filter) to derive a
   more accurate sensitivity function.

ToO Information

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ToO Activators List

• ---(Empty)---

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• ---(Empty)---

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 ?

• YES

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 ?

• N/A

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 prepared your finding charts with tools other than FIMS,
 do they comply with the specifications on the FORS1 Phase 2 web page ?

• YES