README web version of /home/usg/OPS/MTS/readme_xml/readme_71044206

Principal Investigator Email Address

• linda@mpe.mpg.de

Estimated Total Execution Time (hours, including overheads)

• 26h57m04s

General Description

• This run completes our Large Program, and is an H-band medium resolution
   spectroscopy program to derive stellar dynamics (velocity dispersions and rotation)
   close to the AGN in a sample of IR-excess QSOs and IR-luminous mergers.  For each
   source we observe along two orthogonal position angles to determine the rotational
   component of the stars as well as the velocity dispersion.  We submit 1-3 OBs per
   slit, each of which runs just shy of 1 hour. We use a slightly different nod throw
   for each OB to move the source in the detector (together with a 10" dither box).
    In most cases we have used a central wavelength that allows us to observe several
   of the COdelta_v=3 lines as well as the [FeII] emission line.  For sources with
   redshift >0.1, however, this is not possible, since [FeII] falls into the region
   of low atmospheric transmission.  Some OB target coordinates are updated from Phase
   1:  They are now based on deep IR observations of the targets. The PG QSOs are new
   sources, approved as additions to our Large Program by the OPC in period 75.  They
   are not in the original Phase 1 target list:  further information is available from
   VISAS.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• We require excellent seeing conditions (<0.6") in order to screen against
   the (hot dust) emission from the bright compact central engine.  This is necessary
   to measure the weak stellar sbsorption features of the host galaxy close to the
   AGN.

Time-Critical Aspects

• none

Special Execution Requirements

• ---(Empty)---

Special Calibration Information

• We have a preference that the telluric standards be hot, early-type stars
   (B2 or earlier if possible). We, of course, accept solar-type stars if they are
   more convenient for a given OB.  We have included night flats at the end of each
   OB, since our absorption features are ~1-2% of the continuum.

ToO Information

• Not a ToO program

ToO Activators List

• ---(Empty)---

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• No pre-imaging is required for this program.

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 ?

• N/A

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

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

If you are doing spectroscopy, did you draw the slit on the Finding Charts
 ?

• YES

Did you enter the magnitude of the brightest star in the field-of-view
 in each OB ?

• N/A

If you use the MoveToPixel acquisition, have you given clear instructions
 on the FC and in the OB comment section as to how the field should be centered ?

• N/A