README web version of /home/usg/OPS/MTS/readme_xml/readme_76055901
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
he list of OB and target infos are as follows, for the entire runs of
076.C-0559(B)
OB names R (NGS) target separation comments
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PSF_CE284 ~11.5 K=9.4 target = NGS PSF cal for TW Hya
SCI_TWHya_P00 11.4 K=7.4 target = NGC IFU PA=0
SCI_TWHya_P90 11.4 K=7.4 target = NGC IFU PA=90
SCI_51Oph_P00 4.8 K=4.3 target = NGC IFU PA=00
SCI_51Oph_P90 4.8 K=4.3 target = NGC IFU PA=90
SCI_HD141569A 7.2 K=7.0 target = NGC IFU PA=90
The purpose of the observation is to measure the size of circumstellar disks with
spectral PSF differential technique. The spectral PSF could detect any spatially
extended structure down to 1/100 of the intrinsic PSF size, by comparing PSF in
and out of the emission feature (in the present project, CO bandhead emission).
Because the spatial resolution and the sampling is important for the observation,
we will ask two slitlet positions, each perpendicular to the other, for the objects
which the disk orientation (P.A. on the sky) is not well understood. This is because
the spatial resolution of SINFONI is better along the slitlet length, but less,
perpendicular to it.
the DIT is intentionally reduced from the optimal values for the photometric high
s/n (for instance, the pixel counts never reaches about 2/3 of the detector linearity
limit). This is because we want to avoid the off-linear regime, even for 10% or
less. the jitter box size is intentionally set 0, because, we would like to observe
the target always in the center of a slitlets (we want the centroid of the PSF to
be at the center of the slitlet, and not to cross two slitlets.
the target 51 Oph is bright, and possiblly saturate the detector slightly when the
seeing is as good as 0.4 at visible wavelength.
Waiver Requests
Critical Observing Condition Constraints
Time-Critical Aspects
Special Execution Requirements
Special Calibration Information
ToO Information
ToO Activators List
Is this a Pre-imaging run ?
Pre-imaging Requirements
Source(s) of Pre-imaging
Pre-imaging sources not listed above
Do all your OBs comply with the instrument-specific requirements listed
on the instrument-specific Phase 2 web page ?
If this is a pre-imaging run, did you select PRE-IMAGING for the Observing
Category for each Observing Template ?
Do all your finding charts comply with both the general and instrument-specific
Phase 2 Web Pages ?
If you submitted OBs for standard stars, did you specify the magnitude
and spectral type of all standard stars in the OBs ?
Have you included OBs for any calibrations that you need but which are
not part of the Calibration Plan ?
If you are observing Moving Targets, have you attached suitable ephemeris
files to your OBs?
If you have preferences which OBs should be executed first, did you make
use of the User Priority field in the OBs ?
If this is a run that requires coordinated observations with other facilities,
did you give proper instructions in the Time-Critical Aspects Section ?
Did you indicate the magnitude of the brightest object in the field in
each SINFONI OB?
If you are using the AO: Did you indicate for every OB the magnitude
of the guide star, and its distance to the target (if any)?
If you submitted OBs for standard stars, did you use the provided StandardStar
templates?
If you are using a specific offset pattern or position angle: did you
check carefully the definition in the manual?
Did you make really sure that none of your OBs ever saturates the detector?
If you are using the AO: did you enter the correct Strehl Ratio (on-axis,
K-band) AND the seeing value in the constraint set?
Last creation of page: Tue Oct 6 15:40:10 2009
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