README web version of /home/usg/OPS/MTS/readme_xml/readme_82062701

Principal Investigator Email Address

```
skraus@mpifr-bonn.mpg.de
```

Estimated Total Execution Time (hours, including overheads)

```
6.2
```

General Description

The aim of this programme is to obtain high-resolution spectroscopy of
 the Brackett-Gamma 2.166 micron line emission of a sample of 11 T Tauri and Herbig
 Ae/Be stars, complementing VLTI/AMBER spectro-interferometric observations which
 are also scheduled for P83.  All target stars are relatively bright at visual and
 near-infrared wavelengths and can be used as AO and SV guide stars.

To record the Brackett-gamma line, we selected the standard wavelength setting with
 reference wavelength 2150.0 nm (order number 26).  If, due to strong Doppler broadening
 or grating positioning uncertainties, the line wings should be truncated, please
 adjust the wavelength range accordingly (e.g. using free wavelength setting 2153.0,
 grating order number 26).

Since we use a narrow slit of width 0.2", please center the star very accurately
 onto the slit in order to feed sufficient flux into the spectrograph.

*** PLEASE NOTE FOR TTauN, MWC166, and AS205A:
TTauN, MWC166, and AS205A are known to have close companions:
(a) TTauN (V=9.6, H=6.2, K=5.7) is known to have two companions, located 0.7" towards
 the south (PA=185 deg, Delta-K=3.1, invisible at visual wavelengths).
(b) MWC166 (V=7.0, H=6.2, K=6.1) has one companion, located 0.65" towards the north-west
 (PA=298 deg, Delta-V=1.4, Delta-K=3.5).
(c) AS205A (V=13.2, H=6.9, K=6.2) has one companion (AS205B), located 1.3" towards
 the south (PA=212 deg, Delta-V=1.5, Delta-K=0.8).
In all cases, we have oriented the slit perpendicular to the binary separation vector.
  Please center the slit on the main component (brightest star in the field).

For TTauN and AS205A, we have prepared additional finding charts, showing the system
 at higher resolution.

Waiver Requests

In the webletters for the associated AMBER run, three of the proposed
 targets (MWC~758, CQ~Tau, NX~Pup) were marked as technically not feasible for VLTI/AMBER.
  Therefore, we send a TargetChangeRequest, in which three replacement targets were
 approved (MWC~166, AS205A, MWC~863, approved on 2008-07-25).

For the CRIRES observing run, we send a Waiver Request on 2008-07-28, asking to
 change from the "noAO" to the "NGS-AO" mode (approved on 2008-08-04).

Critical Observing Condition Constraints

```
None.
```

Time-Critical Aspects

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None.
```

Special Execution Requirements

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None.
```

Special Calibration Information

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None.
```

ToO Information

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None.
```

ToO Activators List

```
None.
```

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?

Do any OBs include wavelength or flatfield calibrations?

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?

```
N/A
```

Last creation of page: Tue Oct 6 15:40:27 2009
If you have comments, please contact usd-help@eso.org