README web version of /home/usg/OPS/MTS/readme_xml/readme_60907200

Principal Investigator Email Address

• pen@phys.au.dk

Estimated Total Execution Time (hours, including overheads)

• 3h

General Description

• We propose to observe the three sulphur lines at 1045 nm in spectra of
   metal-poor turnoff stars. 
  The S abundances derived will be used to check whether S has a similar overabundance
   with respect to Fe as other alpha capture elements (Mg, Si and Ca).  
  High S/N (>= 200) and high resolution (>50000) are required. The observations
   also serve as a stringent test for flat fielding of CRIRES. Additionally, comparison
   with previously obtained UVES data will allow a comparison of the performance of
   CRIRES and UVES in the overlap region.
  
  CD-30_18140 and HD215801 have higher priority.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• None

Time-Critical Aspects

• None

Special Execution Requirements

• From Francesca - I use this special section to cut&paste the email
   that Poul Erik Nissen sent to Ulli with explanations on how to perform the observations
   - most of this info may be redundant, but in case of need it is better to have it
   -
  
  With the following set up of
  the ETC:
  
  Spectral type F5V
  Point source magnitude V=10
  Slit width 0.4 arcsec
  Seeing 1.0 arcsec
  Airmass 1.2
  Reference wavelength 1046 nm
  Detector integration time 1200 sec,
  
  I now get a slit transmission factor of 0.41 (sounds reasonable)
  and an object signal in PSF of 70303 electrons. From the square root
  of that, one expects a S/N of 265. Taking into account that the
  exposure should preferentially be split into three (NDIT=3) there
  may be some contribution of read-out noise, but still it should be
  possible to obtain S/N > 200. If the seeing is worser than 1 arcsec,
  I suggest to use an entrance slit of 0.6 arcsec corresponding to
  R=33000, which is still acceptable. With setting and readout, I
  suppose this will only allow you to observe the first two of the
  three stars listed in the application:
  
      Star         alpha (2000) delta      V     DIT    NDIT
  CD-30_18140    20 44 06.3   -30 00 08   9.95  400sec   3
  HD 215801      22 48 29.4   -46 03 51  10.04  400 -    3
  G 29-23        23 19 40.4   +03 22 17  10.19  400 -    3
  
  Francesca suggested to observe a hot star for calibration purposes.
  Although there should not be any telluric lines near the sulphur lines
  there are a few in the whole spectral range covered (1031 - 1056 nm).
  Furthermore, the  B star would serve as a way of correcting possible
  flat fielding problems. A good calibrator would be the B3V star:
  
      Star         alpha (2000) delta      V     DIT    NDIT
     HR9006      23 47 16.0   -50 13 35   5.16   60sec    3
  
  This should give superior S/N, but saturation (non-linearity of
  detector) should of course be avoided, so the exposure time may
  have to be shorter. In addition, we should have a sufficient number
  of flat fields allowing calibration of each pixel to S/N > 200, and
  a well exposed ThAr.

Special Calibration Information

• None

ToO Information

• N/A

ToO Activators List

• ---(Empty)---

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