README web version of /home/usg/OPS/MTS/readme_xml/readme_78035501

Principal Investigator Email Address

• akaufer@eso.org

Estimated Total Execution Time (hours, including overheads)

• 02:26:42 (2.5 hrs OPC approved)

General Description

• This FEROS observing run is to support the interferometric monitoring
   of the bright late B-type supergiant beta Orionis (Rigel). The interferometric monitoring
   is carried out with AMBER at the VLTI in the Br gamma line with high spectral resolution
   (R=10000).
  The FEROS observations are supposed to provide complementary information in the
   optical spectrum, in particular the Halpha and higher Balmer lines.
  
  The scientific goal of these observations is to constrain for the first time interferometrically
   the actual extent and spatial distribution of the circumstellar wind structures
   in a massive supergiant, which have been established from optical spectroscopic
   monitioring observations similar to the FEROS observations requested here.

Waiver Requests

• No Waiver Request was submitted (except for late phase 2 submission)

Critical Observing Condition Constraints

• The observing conditions constraints are very relaxed for the FEROS observations
   due to the overwhelming brightness of the target. 
  Observations through thin clouds and at high airmass can be compensated by slight
   adjustments of the exposure time which is about 1 second.  A S/N at Halpha of about
   300 is needed.

Time-Critical Aspects

• The execution of the 18 submitted OBs should be distributed over the whole
   observing period from October to March. 
  A minimum of 3 days between the consecutive execution of two OBs is required.
  
  According to the P78 schedule, 9 service mode blocks are available at the 2.2m over
   the 6 months, i.e.,
  2 OBs should be executed per service mode block with at least 3 days between the
   two OBs.

Special Execution Requirements

• The ETC estimate of 1 second exposure time to achieve a S/N of 300 at
   Halpha is quite rough and will depend critically on the actual observing conditions.
   Main limitation will be the ability to center the very bright target on the fiber
   entrance.
  Therefore, please adjust the exposure time to achieve a minimum S/N of 300 while
   not saturating the detector.

Special Calibration Information

• standard calibrations are sufficient

ToO Information

• N/A

ToO Activators List

• N/A

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• N/A

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 ?

• 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

Did you set 'New Preset' flag in all acquisition templates to 'True'?

• YES

If you use any lamp, did you check that it should never be left on at
 the end of any OB?

• N/A