README web version of /home/usg/OPS/MTS/readme_xml/readme_81021900

Principal Investigator Email Address

• smengel@eso.org

Estimated Total Execution Time (hours, including overheads)

• 08:26:28

General Description

• The goal of this project is to determine radial velocities of stars in
   the massive young MW cluster Westerlund 1. Radial velocities for the hot stellar
   types are determined from Brg absorption lines (and other lines in the region of
   setting 2.145 micron). The 2.31 micron setting targets red supergiants and yellow
   hypergiants.
  In order to obtain spectra for as many stars as possible in the magnitude range
   mK=7-11, we are stepping the slit across the cluster (avoiding stars brighter than
   ~5th mag).
  The long execution time (probably overestimated by ETRM) means that we split this
   up into 4 OBs, which can be executed completely independently per epoch.
  In order to find/evaluate variations in radial velocity (through binarity in the
   hot stars, or radial pulsations in the YHGs), we have submitted OBs for 2 epochs.
   Please, try to have at least 1-2 weeks go by between each Epoch1 and Epoch2 pair
   of OBs. At least, under no circumstances, execute the two epochs for the same field
   within the same night.
  
  There are no critical constraints for this program, but the seeing should NOT be
   too good.
  We have taken care to avoid the brightest stars in our spectroscopy setup, and use
   two distant NB filters for the acquisition, but if the seeing is 0.6" or better,
   these measures might not be good enough to avoid saturation.
  
  The exeuction is as follows:
  Star W9 (marked with a circle in FCs) is always the acquisition object. From there,
   an initial blind offset is applied (mostly along the slit for fields 1 and 2, and
   also perpendicular to the slit for fields 3 and 4). From there, the scanning starts
   in 2.145 micron, sometimes with a gap for a bright star. After the scanning, the
   grating is moved to 2.31 micron, and starting from the origin, 9 individual stars
   are observed (2 individual templates, left and right of the original slit position,
   in order not to accumulate too many offset uncertainties).
  
  It is normal that many positions will not include a target. But if it is apparent
   that an offset goes in the wrong direction, or saturation occurs (because we are
   getting too close to one of the bright stars), or one of the 2.31 micron frames
   does not include a star, please contact USD.
  
  The brightest star in the finding charts has mK~2, next-brightest mK~3-3.5. The
   brightest stars which are included in our 2.145 spectra are mK~5.
  
  For our purposes, the data should be self-calibrating regarding telluric standards.

Waiver Requests

• We asked permission to submit OBs including two different central wavelengths,
   and to violate the 1-minute-per-position-rule.
  Both requests were granted (081.D-0219A.01.WAV, 12.02.08)

Critical Observing Condition Constraints

• None.
  Seeing should not be better than ~0.6". Best would be DIMM between 1-1.8"

Time-Critical Aspects

• Between each pair of OBs for a given field, at least 1-2 weeks should
   pass between Epoch 1 and Epoch 2.
  
  The pairs are:
  
  Wd1_1_Epoch1	Wd1_1_Epoch2
  Wd1_2_Epoch1	Wd1_2_Epoch2
  Wd1_3_Epoch1	Wd1_3_Epoch2
  Wd1_4_Epoch1	Wd1_4_Epoch2
  
  Otherwise, there are no timing constraints. There's no maximum time between epochs,
   and the fields
  are independent.

Special Execution Requirements

• None

Special Calibration Information

• For our purposes, data should be self-calibrating wrt telluric standards
   (different stellar types included in spectra, which can serve as telluric standards
   for the other stellar types in the different wavelength ranges).

ToO Information

• ---(Empty)---

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 ?

• 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

If you submitted OBs for standard stars, did you use the provided StandardStar
 templates ?

• N/A

If you are using a specific offset pattern or position angle, did you
 check carefully the definition in the manual ?

• YES

If you are doing spectroscopy, did you draw the slit on the Finding Charts
 ?

• YES

Did you enter the magnitude of the brightest star in the field-of-view
 in the 'Instrument Comments' field of each OB ?

• YES

If you use the MoveToPixel acquisition, have you given clear instructions
 on the FC and in the OB comment section as to how the field should be centered ?

• N/A