README web version of /home/usg/OPS/MTS/readme_xml/readme_84111507

Principal Investigator Email Address

• labadie@iac.es

Estimated Total Execution Time (hours, including overheads)

• 1.33

General Description

• - This is an imaging run of the debris disk star HD141891 in the N and
   Q bands, using SIC and Q2 filters. Note that acquisition should be done in K (see
   Special Execution requirements).
  - Appropriate period for observing HD141891 in optimal conditions is the second-half
   of March.
  - We request standard calibration for this run to be used also as PSF-reference
   images.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• For this imaging run, we necessitate high angular resolution:
  1) Thus we need to be diffracion-limited at 10 microns, which occurs with a seeing
   of 0.8" in the optical.
  2) Since we image faint structure, we necessitate optimal atmospheric conditions
   (photometric) in order to have minimum flux losses.

Time-Critical Aspects

• For our science, we necessitate to be close to the diffraction limit in
   the N band. Thus, we requested lowest possible airmasses. For HD141891, we wish
   to have observations below 1.3 airmass (which happens during 1h40min) or 1.4 airmass
   (which happens during 4h20min) at periods indicated in Time Intervals, with a preference
   towards end of March.

Special Execution Requirements

• According to IPAC catalog (http://nsted.ipac.caltech.edu), HD141891 and
   IRAS-15507-6316 are the same target with fluxes N~6 Jy and Q~1.6 Jy, with indication
   of being "slightly contaminated by companions". 
  At the contrary, according to SIMBAD HD141891 and IRAS-15507-6316 are different
   targets distant by 9".
  
  In order to solve this indetermination, we suggest to precisely acquire the source
   in the K-band, where HD141891 appears as the brighter source in the field (see 2-MASS
   Finding Chart, and K~2.1), then to switch to the SIC filter once the acquisition
   is done.
  
  Also, in order to perform appropriate centering of the 20 mu image on the 10 mu
   image at the pointing accuracy of the telescope during the data reduction phase,
   it is mandatory that 20 mu images are done immediately after the 10 mu images. N
   band and Q band imaging must not be separated in time.

Special Calibration Information

• For this run, we use as a PSF-reference star:
  
  - We need to have the star HD151249 observed at similar airmass than the science
   target, which occurs directly AFTER the science observation. We submitted a corresponding
   calibration OB.
  
  - HD151249 brightness is N~34 Jy and Q~13 Jy.

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 ?

• 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?

• YES

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

• YES