README web version of /home/usg/OPS/MTS/readme_xml/readme_83082401

Principal Investigator Email Address

• stumpf@mpia-hd.mpg.de

Estimated Total Execution Time (hours, including overheads)

• 2 h

General Description

• This is a spectroscopic run for only one target (binary brown dwarf) in
   the Ks filter. The brighter component Kelu1 A has K=12.32 and the fainter component
   K=12.75. Since the target is too faint in R-band we will use 2MASS 130539-254129
   (S201113311069) as AO guide star (R=14.5) as well as SVGS (K=12.13), coordinates
   are for Epoch 2000.0  
   
  Acquisition:
  ------------
  
  ATTENTION: 
  Due to the relatively large offset between our target and the SVGS the binary components
   need to be moved slightly upwards in the slit, so that target and SVGS fit on the
   slit view detector. Therfore we calculated a Pointing position(= no real target)
   between target and SVGS which should be placed in the center of the slit. The corresponding
   coordinates are provided in the target box of the OB. This should also lead to the
   alignement of both!! target binary components in the slit during acquisition. If
   this procedure works out there should be still ~8.3" distance between Kelu-1 and
   the upper end of the detector which would provide enough space for the given noddthrow.
  To fit both Kelu-1 components in the slit, the position angle of the slit has to
   be 42.9 degrees! PLEASE make shure that both! binary components stay in the slit
   during the whole observation!!!!! 
  
  The coordinates for the target Kelu-1 AB calculated for Epoch 2009 are
          RA: 13 05 40.007  and   DEC: -25 41 06.7  
  and are also provided on each Finding Chart. Kelu-1AB is a higher proper motion
   object with pmRa ~0.285"/yr and pmDEC ~0.03"/yr (also provided in the target box).
   The offset calculated between target and SVGS for Epoch 2009.0 will be ~ -12.39"
   in RA and -22.5" in DEC. Depending on the time of observation the RA/DEC offsets
   will slightly change. PLEASE always! verify after aligning the given Pointing position
   in the slit center, that both Kelu-1 components are really in the slit!
  
  We provide 3 Finding Charts (including a 2'x2' and a magnified one) for the science
   OBs with all relevant coordinates and the slit orientation. The red dot on the slit
   shows the calculated Pointing Position and should correspond to the slit center
   as given in the manual.
  
  OBSERVATION:
  ------------
  We will use the 25/1/i wavelength setting (central wavelength= 2293.2nm) with the
   0.2" slit. With a separation of the binary components of ~0.38" it should be possible
   to spatially resolve the 2 spectra. For a sufficient accuracy of our RV measurement,
   a S/N ratio ~30 for the fainter component Kelu1 B is required. To achieve a very
   precise RV determination we will use simultaneously the N2O gas-cell as a wavelength
   reference. Additionally we will observe 1 nodding cycle without the cell to receive
   a reference template. The same principle will be performed during the calibration
   OB for a telluric standart.
  
  PLEASE be also aware about the critical observing condition constrains and the special
   calibration information for this run!!! (As described therein)
  
  
  Beside our own telluric standart calibration OB, normal standart calibration for
   bias, arcs and flats provided by ESO are sufficient. Nevertheless, if we could get
   one set of flats with the N2O cell infront. That would help a lot with data reduction.
  
  THANK you very much for your support concerning all the different issues of this
   run!!!!

Waiver Requests

• waiver request with WaiverID 383.C-0824(B) 
  for the science OB (Kelu1) with a total execution time of 1:45:00 
  was submitted January 23rd 2009 at 4:10 pm
  and approved January 26th 2009 at 1:51 pm

Critical Observing Condition Constraints

• If it should turn out that due to the higher proper motion of the target,
   the calculated Pointing position is not accurate enough to aligne both binary components
   in the slit  and still include the SVGS in the FoV, please feel free to adjust the
   parameters accordingly.
  
  If in the end the AO guide star does not work out as SVGS (due to distance to target
   and slit orientation), one could also try to use the brighter component of the binary
   target (Kelu1 A) as the SVGS (binary component distance = 0.38"). It should be bright
   enough (K=12.32). In this case please check carefully if the binary itself prevents
   the slit-view system to operate correctly or if it offsets the target from the slit!
    
  
  If this should also fail, it would be still worth trying to use CRIRES without AO
   and the 0.4" slit (adjusting the DITs in the science and calibration OB accordingly!!).

Time-Critical Aspects

• N/A

Special Execution Requirements

• N/A

Special Calibration Information

• We added a calibration OB:
  CAL_telluric_standard to be able to perform telluric correction during data reduction.
   We chose the standart HIP 68269 (B8V) with R=5.24 and K=5.38 and a S/N ratio of
   159@2293.2nm. 
  The telluric standard is bright enough to serve as AO and SVGS. Please execute this
   OB right after the science OB. Please be aware that the slit orientation has to
   be the same as for the science OB (as indicated in the OB). We will obtain (in the
   same way as for the science OB) one dataset with the N2O gas-cell and one without
   (as reference template). 
  If possible, please place the telluric standart at the same position on the science
   detector as Kelu1 (=science target) in the OB before. This will ease any necessary
   correction of the science data.
  If it turns out to be necessary to change the telluric standard, a range between
   B4-A0 will be acceptable. Nevertheless it is very important!!!! to observe at nearly
   the same airmass as the science object.

ToO Information

• N/A

ToO Activators List

• N/A

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?

• YES

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?

• YES

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?

• N/A