README web version of /home/usg/OPS/MTS/readme_xml/readme_84082100

Principal Investigator Email Address

• boekel@mpia.de

Estimated Total Execution Time (hours, including overheads)

• 6.0

General Description

• The purpose of this programme is to obtain a deep, high resolution VISIR
   spectrum
  of DG Tau and it's jet, to reveal the spatial origin and kinimatics of the 
  12.81 micron [NeII] emission line. To this purpose we will place a long slit over
   
  the central point source (continuum dust emission from the disk), oriented along
  the jet direction (~46 degrees E of N).
  As the [NeII] observations are very challenging from a sensitivity point of
  view, a number of integrations are needed to build up SNR.
  
  The 
  
  Additionally, an optical UVES spectrum of the jet (with the same slit orientation)
  will yield the spatial distribution of a number of optical (forbidden) emission
  lines that trace the jet density and excitation conditions.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• none other than given in "constraint set" in the OB

Time-Critical Aspects

• The timing of the observations is not critical.
  
  However, it would be good if the complete integration (6 OBs of 1 hour) would be
   executed over
  a not too long period - if possible within 1 or 2 VISIR service block(s). The UVES
   spectrum 
  would preferably be taken around the same time (not necessarily within the same
   night, but within
  1 or 2 weeks).

Special Execution Requirements

• It is important to accurately center the central point source in the slit,
   since
  we will combine multiple measurements (to build up SNR) that should essentially
  have the same slit position/orientation.
  
  DG Tau has a continuum flux of ~4 Jy at 12.8 micron. That should result in a
  ~300 sigma detection in the prescribed 120 second exposure of the acquisition
  template. That ought to be sufficient for an accurate centroid determination,
  and thus for a proper ad-hoc alignment of the individual observations.
  
  Note that DG Tau is the brightest star in its immediate surroundings, with
  V=12.8 it just falls within the V=11-13 brightness range for guide stars of
  VLT observations (though it is somewhat fainter than the V=12 that is asked
  for in the last check-box below, hence the "no" there).
  Further magnitudes of DG Tau: R=11.4, H=7.7, K=7.0, 12.8 micron ~4 Jy.

Special Calibration Information

• ---(Empty)---

ToO Information

• ---(Empty)---

ToO Activators List

• ---(Empty)---

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• ---(Empty)---

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 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?

• YES

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

• NO