README web version of /home/usg/OPS/MTS/readme_xml/readme_82504301

Principal Investigator Email Address

• jgroh@mpifr-bonn.mpg.de

Estimated Total Execution Time (hours, including overheads)

• 1:59:35

General Description

• The goal of the program is to obtain *spatially-resolved* spectra of Eta
   Carinae and its inner nebula after the periastron passage of the companion in January
   and early February 2009. For each reference wavelength the slit should be centered
   on the central star, with a position angle of 325. Note that this PA is slightly
   misaligned (8 degrees) relative to the major axis of the nebula (see finding chart
   1). Finding chart 1 shows how the star+nebula should look in the CRIRES acqisition
   image (image is saturated in this case). After the slit in centered on the central
   star, 1s exposures repeated NDIT times should be made in order to not saturate the
   spectrum of the central star. A large number of NDIT (17-25 depending on the reference
   wavelength) should be used in order to build up the desired high S/N. After that,
   longer exposures of 41-55s (depending on the reference wavelength) should be made
   at specific offset positions from the central star in order to obtain the spectrum
   of the nebula. The offset positions for the long exposures should be, in DETECTOR
   coordinates:
  -grating angle 26, both ref. wave. 2150.0 and 2156.5: (X,Y)=(-0.2,0), (X,Y)=(-0.2,0),
   (X,Y)=(0.6,0), and (X,Y)=(0.2,0). 
  -grating angle 27, both ref. wave. 2070.4 and 2076.6: (X,Y)=(-0.2,0), (X,Y)=(-0.2,0),
   (X,Y)=(0.6,0), (X,Y)=(0.2,0) and (X,Y)=(20,0).
  -grating angle 52, both ref. wave. 1087.3 and 1090.4: (X,Y)=(0.2,0), (X,Y)=(0.2,0),
   (X,Y)=(0.4,0) , (X,Y)=(-1.0,0), (X,Y)=(-0.2,0), (X,Y)=(-0.4,0), and (X,Y)=(20,0).
  
  Note that the above offsets are cumulative from the previous one (i.e. we are assuming
   that the telescope is not returning to 0,0 after each offset position). The absolute
   offsets *relative to the central star* in detector coordinates (shown in Finding
   chart 2 for each OB), corresponding to the cummulative offsets given above, are:
  -grating angle 26, both ref. wave. 2150.0 and 2156.5: (X,Y)=(-0.2,0), (X,Y)=(-0.4,0),
   (X,Y)=(0.2,0), and (X,Y)=(0.4,0). 
  -grating angle 27, both ref. wave. 2070.4 and 2076.6: (X,Y)=(-0.2,0), (X,Y)=(-0.4,0),
   (X,Y)=(0.2,0), (X,Y)=(0.4,0), and (X,Y)=(20.4,0).
  -grating angle 52, both ref. wave. 1087.3 and 1090.4: (X,Y)=(0.2,0), (X,Y)=(0.4,0),
   (X,Y)=(0.8,0) , (X,Y)=(-0.2,0), (X,Y)=(-0.4,0), (X,Y)=(-0.8,0), and (X,Y)=(19.2,0).

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• There are no critical observing constraints other than those specified
   in each OB.

Time-Critical Aspects

• The OBs should be observed as soon as possible (late Jan/early Feb 2009)
   after the CRIRES intervention.

Special Execution Requirements

• None.

Special Calibration Information

• A telluric star should be observed following the science OB only for grating
   angle 27. For grating angles 26 and 52 there is only few weak telluric lines which
   will not affect our observations.

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?

• 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