README web version of /home/usg/OPS/MTS/readme_xml/readme_76055900
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
the list of OB and target infos are as follows, for the entire runs of
0559(A)
OB names R (NGS) target separation comments
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PSF_HD-285204 ~10.0 K~7.8 target = NGS PSF cal for LkCa 15. spt=K5
PSF_StKM_1-440 11.2 K=10.0 target = NGS PSF cal for DG Tau/GG Tau
spt=K5
SCI_DG_Tau 10.6 K= 6.8 target = NGC IFU PA=46
SCI_GG_Tau_A 10.8 K=7.3 target = NGC IFU PA=5
SCI_LkCa_15 11.48 K=7.6 target = NGC IFU PA=-24
The purpose of the observation is to measure the size of circumstellar disks with
spectral PSF differential technique. The spectral PSF method could detect any spatially
extended structure down to 1/100 of the actual PSF size, by comparing PSF in and
out of the emission feature (in the present project, CO bandhead emission at 2.295
um).
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 to 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 over the two slitlets.
the PSF calibration stars are chosen so that the spectral type is similar to that
of the objects. means cannot be used as atmospheric standard. we need and request
separate atmospheric standard stars.
Waiver Requests
Critical Observing Condition Constraints
Time-Critical Aspects
Special Execution Requirements
we need PSF calibration observation. Since PSF is subject to the brightness
of wavefront reference, and also the exposure time, we prepared calibration stars
whose magnitude at the wavelength of wavefront measurements is almost same with
the objects. we notified when the OBs for PSF calibration is supposed to be executed
in the user comments so that the airmass matches best to the particular objects.
not all the objects have PSF calibration stars. partly because PSF is no longer
the function of brightness at the bright end of the stars, and because in principle,
PSF can be also calibrated by the object itself.
the jitter box size is intentionally set to 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 over the two slitlets.
Special Calibration Information
The HD 285204 and StKM 1-440 are the PSF calibration stars. HD 285204
is selected so that the airmass is about same with LkHa 15, after the observation
of that object star. So, please observe HD 285204 immediately after LkHa 15.
We understand the PSF stars are usually obtained only after the objects are observed.
However, the purpose of observing PSF star is to monitor the temporal variation
of the PSF, and make sure the instrumental PSF does not differ (or does differ)
as much as it affects on the main result. In case the PSF varries slowly, but linearly
over the night, the PSF ovservation only after the objects may be subject to a systematic
trend. So, we would like to observe one PSF star after the object and another before
that, namely, StKM 1-440 before DG Tau. We meant the ideal sequence may be StKM
1-440 => DG Tau => GG Tau, in terms of airmass matching, however, observing
GG Tau in the same sequence is not essential (coupling StKM 1-440 with DG Tau is
more relevant for us), we would appreciate if the night astronomer could take care
of StKM 1-440 => DG Tau sequence, because they do not take 40 min. in total.
the PSF calibration stars are chosen so that the spectral type is similar to that
of the objects. means cannot be used as atmospheric standard. we need and request
separate atmospheric standard stars.
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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