README web version of /home/usg/OPS/MTS/readme_xml/readme_77070602

Principal Investigator Email Address

• Fabien.Malbet@obs.ujf-grenoble.fr

Estimated Total Execution Time (hours, including overheads)

• 2

General Description

• Recently, Thi et al. (2005, A&A 430, L61) have found that hot and
   dense CO gas is located in the inner AU of a Keplerian disk around 51Oph (see Fig.
   4 of our proposal). We want to observe 51 Oph in the spectral region where the CO
   bands are preeminent, i.e. [2.28-2.40] microns. The goal is to detect if there is
   a change in the amplitude of the visibility compared to the continuum. If positive,
   this will give us indication of a different size of the CO gas emission compared
   to the dust emission (very similar to what has been presented with early AMBER results
   on MWC 297 at the ESO-EII workshop, astro-ph/0507226 but for the disk and wind emission
   in the Brackett gamma line). The triplet UT1-UT2-UT4 give us both the largest baseline
   and a short one at different position angle. The spectral range to be observed is:
   [2.27-2.35] to get the continuum and the v=2-0 and v=3-1 CO transition. If the coherence
   time is fast it could be reduced to the continuum and v=2-0 [2.28,2.32] (see special
   execution requirements). The observation should be done at HA typically in the range
   [-0h30,2h] the best time being in the range [0h30-1h] (see time-critical requirements).

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• Seeing better than 1.2"

Time-Critical Aspects

• The observation should be done at HA typically in the range [-0h30,2h]
   the best time being in the range [0h30-1h]. We specified the largest HA range in
   the OB with sideral range: [17:01,19:31].

Special Execution Requirements

• The spectral range to be observed is: [2.27-2.35] to get both the continuum
   and the v=2-0 & V=3-1 CO transitionS. This setup requires 50ms DIT and therefore
   decent observing conditions.
  If the coherence time is fast it can be reduced to [2.28,2.32] and 25ms DIT.

Special Calibration Information

• The Calibrator is not from CalVin.
  
  It was obtained from ASPRO: HD 165185 (18 06 23.7193 -36 01 11.239)
  V=5.95, K=4.47
  SpT=G3V
  Expected Diameter: 0.585+/-0.040

ToO Information

• None

ToO Activators List

• None

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• None

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 ?

• 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

Did you indicate for each science star OB the corresponding calibrator
 star OB (and vice versa) in the 'Instrument Comments' field ?

• YES

If you use calibrator stars which are not in the CalVin database, did
 you specify their characteristics in the README file and in the OBs ?

• YES