README web version of /home/usg/OPS/MTS/readme_xml/readme_84052700

Principal Investigator Email Address

• mmoerche@eso.org

Estimated Total Execution Time (hours, including overheads)

• 8

General Description

• This program aims to detect [NeII] emission associated with a T-Tauri
   star, Glass I.  We aim to test/confirm that the disk (likely edge-on) is the source
   of the [NeII] emission, and compare it to the Spitzer-observed line flux to see
   if the line emission is coincident with the continuum emission.  We will also be
   looking for extended emission along the slit, specifically with our one OB that
   uses a wide slit (1").  Finally, we will be looking for a spectroastrometric signature
   of the [NeII] emission, and to do this we will observe at 4 PAs separated by 90
   degrees each, such that two pairs of parallel/anti-parallel slit positions are employed
   (one set along the binary pair and the other perpendicular to it).

Waiver Requests

• We have submitted two waiver requests:
  
  1- to exceed 1-hour execution time per OB (submitted 31 July 2009)
  
  2- to have consecutively observed OBs (submitted 31 July 2009)
  
  Both were approved on 4 August 2009.

Critical Observing Condition Constraints

• N/A

Time-Critical Aspects

• N/A

Special Execution Requirements

• There are two pairs of PAs in the program: PA1 (parallel PA and its anti-parallel,
   PA+180) is oriented along the Glass I binary pair, and PA2 (parallel PA and its
   anti-parallel, PA+180) is oriented perpendicular to it.
  
  The OBs in the program have a number and a letter designation:
  + PA1 or PA2 indicates the "set" of PAs (a parallel and and anti-parallel pair)
  + "a" and "b" signify the parallel and anti-parallel within a PA pair
  
  It is critical that the "a" and "b" OBs for each of the PAs (PA1 and PA2) are observed
   consecutively.  This is important for removal of false spectroastrometric signatures.
    Specifically, "GlassI_PA1_a" and "GlassI_PA1_b" must be observed consecutively,
   and likewise for the pair labeled "PA2".
  
  "GlassIa_WideSlit" is a wide-slit observation oriented along the binary to look
   for extended emission. 
  
  Finally, the two sets of OBs at the two PAs should be executed within a few days
   of one another, because the variability of the [NeII] emission is not known.

Special Calibration Information

• A spectroscopic standard should be observed before the Glass I science
   observations.  We have included OBs for Alpha CMa as the telluric standard.  This
   source has three OBs, one for each of the sets of observations (the two OBs at PA1,
   the two OBs at PA2, and the one OB in wide-slit mode).

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 ?

• YES

Have you included OBs for any calibrations that you need but which are
 not part of the Calibration Plan ?

• YES

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

If the provided finding chart is at a different wavelength than the observations,
 did you clearly describe in the README file how to identify the target?

• N/A

Did you specify a guide star brighter than V=12mag within a field of
 r=5arcmin around the science target?

• N/A