README web version of /home/usg/OPS/MTS/readme_xml/readme_84059501

Principal Investigator Email Address

• leen@ster.kuleuven.ac.be

Estimated Total Execution Time (hours, including overheads)

• 7h

General Description

• ---------------------------------------------------------------------
   
  general information 
  ---------------------------------------------------------------------- 
  CRIRES observations will allow us to monitor the upward propagation of the 
  shock wave in the Mira's outer atmosphere and inner wind region by 
  observing the doubling of the 12CO v1-0 R0, R1, R2 and R3 lines with Free setting:
   order 12; lambda 4652.5nm 
  and the 12CO v2-0 R(1), P(1), P(2) lines with Standard Setting: Order:24 , Reference
   
  Wavelength:2361.70 nm
  For R Ceti, metallic lines in the range 2182 to 2190 nm are also targeted.
  
  Observations should be done at light phases differing by about 0.1, at and after
   max light
  
  Each science OB is accompanied by a telluric CAL OB, named in accordance to the
   science OB, and which can be observed either after or before the science OB.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• Critical issues: see special conditions below

Time-Critical Aspects

• Here is the temporal sequence along which the OBs (SCI + CAL) should be
   executed (as indicated in the 'Time intervals' for each OB):
  
  Between     and         OB
  2009-09-30  2009-10-16  R Ceti-october-0  + CAL
  2009-10-26  2009-11-06  R Ceti-october-1  + CAL
  2009-10-30  2009-11-20  omi Cet - november+ CAL
  2009-11-16  2009-11-30  R Ceti-november   + CAL
  2009-11-30  2009-12-20  omi Cet - december+ CAL
  2009-12-16  2009-12-31  R Ceti-december   + CAL
  2009-12-31  2010-01-31  omi Cet - january + CAL
  2010-01-20  2010-01-31  R Ceti-january    + CAL  
  (end of visibility season)
  
  These dates are not to be obeyed strictly; it is to ensure a reasonably regular
   time sampling along the light curve
  (to monitor the evolution of the line shape along the light cycle).
  
  Omi Ceti: Maximum: 2009-11-14 period 332d 
  R Ceti:   Maximum: 2009-08-22 period 166d

Special Execution Requirements

• Caveat:
  For omi Cet, there is the concern of saturating the detector (with a K-band diameter
   of 30 mas, 
  it must be considered a point source for CRIRES).
  Therefore, we have selected the smallest possible slit width (0.05 arcsec) and DIT
   (0.15 sec).
  With these settings (and for Mira at max light), 
  only CCD #2 gets very close to saturation, the other being still above the 
  linearity limit. Nevertheless, we are only interested in the line doubling, not
   the equivalent widths.
  The only concern is with nodding and sky measurement.
  Sky measurement has been scheduled BEFORE the target, to prevent possible remanence.
  However, once on the target, the nodding could possibly spread the pixels with remanence
   all over the chip.
  I do not know whether there is an optimal strategy here.
  
  There is also a concern with Mira B, located 0.6 arcsec to the East of Mira A.
  Working with position angle 0 in SKY mode ensures that all nodding offsets along
   the Y axis will correspond to the
  N-S direction, thus away from Mira B.

Special Calibration Information

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ToO Information

• ---(Empty)---

ToO Activators List

• ---(Empty)---

Do the README file and the instrument comments of the telluric stars
 OBs include the required S/N/pixel of the spectrum of the telluric star, its spectral
 type and allowed spectral range?

• YES

Do any OBs include wavelength or flatfield calibrations?

• NO

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

• N/A

If the slit viewer guide star is different from the target, are the RA
 and DEC offsets accurate to within 0.05 arcsec and do they take into account the
 relative proper motion between the two objects?

• N/A

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

• YES