README web version of /home/usg/OPS/MTS/readme_xml/readme_81504600

Principal Investigator Email Address

• forster@mpe.mpg.de

Estimated Total Execution Time (hours, including overheads)

• 09:59:21.000

General Description

• Information on target and AO TTS:
  
  OB names                 R(TTS)  target  separation  comments
  --------------------------------------------------------------------
  SINS_BX610_LGSAO_DDT81-#  18.0   K=19.2   58 arcsec   H_alpha: line at 2.107um
                                                        integrated flux ~2e-16 erg/s/cm2
                                                        major axis FWHM ~ 1.3"
  
  
  We are using an "on-source dithering" strategy (cf. below), which requires very
  accurate blind offset to the target, to a few pixels at the 100mas scale employed.
  We would like to verify with the data of the first OB that the source positioning
  is as accurate as it should be.
  We therefore wish to request that the OB SINS_BX610_LGSAO_DDT81-0 is first put in
  the observing queue, and that the subsequent OBs (SINS_BX610_LGSAO_DDT81-1 to -5)
  are queued after we have verified the positioning from the data of the first OB.
  
  
  The main characteristics of the observations are as follows.
  
  - The PA is set to 20 deg for the target, Q2343-BX610, primarily for scientific
   reasons
    and to allow for on-source dithering, as well as to ensure the tip-tilt reference
    falls within the Field Selector field of view (FOV).  THIS PA SHOULD NOT BE MODIFIED.
   
  - OBs are named after the target, with "-0", "-1", "-2", etc. appended for different
   OBs.
  - The priority among the OBs is set using the priority flag in the templates, and
   the
    order is reflected in the "-#" used in the OB names.
  
  - The brightest spectral feature of the target is H_alpha in emission;
    the observed wavelength, integrated flux, and size in H_alpha are thus
    given in the table above.
  - We are using the 100mas scale, with FOV of 3.2"x3.2".
    The target is extended mostly in one direction (PA ~ 20 deg).  This morphology
    is best seen in HST/NICMOS imaging at a resolution of ~0.2" (included in the
    finding charts).  The target size enables an "on-source dithering" strategy,
    in which two successive exposures are offset along E-W by about 1/2 the 3.2"x3.2"
    FOV (i.e., about 1.5") for pairwise sky subtraction.  Small jitters about the
   two
    main dithering positions are used to minimize the number of redundant positions.
  
  We would like to note that for this target, the only suitable tip-tilt source (TTS)
  available is a compact but rather faint galaxy.  We are aware of the possible limitations
  this could have on the AO performance.  Our experience from the SINFONI GTO visitor
   runs 
  using AO in LGS mode with TTS of similar magnitude and at comparable distances from
   the
  science targets was successful and provided effective angular resolution of 0.15"-0.3",
   
  which still meets our scientific requirements.
  We are thus confident that these observations can be carried out, and if the acquisition
  presents some difficulties, we would like to kindly ask the observers to do their
   best,
  or to contact the P.I. if needed.
  
  Remarks on the finding charts:
  
  - Three finding charts are provided:
    (1) SINFONI_Q2343-BX610_LGS_fchart1.jpg: has wider FOV; a large and
        a small black square show regions 1' x 1' and 8" x 8" centered on the target;
        the TTS is labeled "R1".  The larger dashed rectangle shows the Strap Field
        Selector FOV of the AO system.
    (2) SINFONI_Q2343-BX610_LGS_fchart2.jpg: is zoomed in on the target, with the
        large and small solid-line squares showing regions of 8" x 8" and 3.2" x 3.2"
        centered on the target.  In addition, two dashed-line squares show the outline
        of the two main dithering positions for Q2343-BX610.
    (3) SINFONI_Q2343-BX610_LGS_fchart3.jpg: similar to above zoomed chart but based
        on much higher resolution HST/NICMOS imaging.  This clearly shows why the
   
        PA = 20 deg is crucial for our target.

Waiver Requests

• One Waiver Request was submitted:
  
  281.A-5046A.01.WAV: for an increase of the OB execution time limit to 1h50.
                      (submitted on Sept. 11, 2008; Approved on Sept. 11, 2008)

Critical Observing Condition Constraints

• Transparency constraints:
  - For all OBs, CLEAR sky transparency conditions is acceptable, as specified
    in the proposal.
  
  Moon constraints:
  - Conforming to our proposal, there is no constraint on lunar phase and so 
    the illumination is set to 1.0.
  - The TTS is faint (V >~ 16), however, so we have set the constraint for 
    moon distance to 50 degrees
    (following recommendations from the ESO SINFONI P2PP Web pages
     http://www.eso.org/observing/p2pp/SINFONI/SINFONI-P2PP.html#Requirements)
  
  Seeing constraints:
  - Seeing <= 0.6", as specified in the proposal.

Time-Critical Aspects

• N/A

Special Execution Requirements

• As we explain in the General Description, we are using an "on-source dithering"
   strategy.
  This requires very accurate blind offset to the target, to a few pixels at the 100mas
  scale employed.  We would like to verify with the data of the first OB that the
   source
  positioning is as accurate as it should be.
  We therefore wish to request that the OB SINS_BX610_LGSAO_DDT81-0 is first put in
   the 
  observing queue, and that the subsequent OBs (SINS_BX610_LGSAO_DDT81-1 to -5) are
   queued 
  after we have verified the positioning from the data of the first OB.
  
  The PA = 20 deg is necessary and essential for our target Q2343-BX610,
  and should not be modified without approval from the PI.
  
  We have also noted in the General Description that the TTS is rather faint.
  While from our experience during previous SINFONI GTO runs we are confident the
   
  observations can be carried out and meet our scientific requirements, please do
   
  not hesitate to contact the PI in case of difficulties.

Special Calibration Information

• N/A

ToO Information

• N/A

ToO Activators List

• N/A

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• N/A

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 ?

• YES

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

Did you indicate the magnitude of the brightest object in the field in
 each SINFONI OB?

• YES

If you are using the AO: Did you indicate for every OB the magnitude
 of the guide star, and its distance to the target (if any)?

• YES

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

Did you make really sure that none of your OBs ever saturates the detector?

• YES

If you are using the AO: did you enter the correct Strehl Ratio (on-axis,
 K-band) AND the seeing value in the constraint set?

• YES