README web version of /home/usg/OPS/MTS/readme_xml/readme_81059200
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
OB names R(NGS) target separation H_alpha
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SA12-6339 14.5 K=20.2 57 arcsec line at 2.164um
flux ~0.1e-16 erg/s/cm2
SA12-8768 16.8 K=20.1 38 arcsec line at 2.092um
flux ~0.9e-16 erg/s/cm2
K20-ID6 ~16 K=19.9 55 arcsec line at 2.124um
flux ~0.6e-16 erg/s/cm2
Q1623-BX376 15.5 K=~20 34 arcsec line at 2.238um
flux ~0.5e-16 erg/s/cm2
Q1623-BX455 16.6 K=21.6 38 arcsec line at 2.237um
flux ~1.9e-16 erg/s/cm2
Q1623-BX502 15.5 K=21.8 8.5 arcsec line at 2.072um
flux ~1.3e-16 erg/s/cm2
Q1623-BX599 17 K=19.9 50 arcesec line at 2.185um
flux ~1.8e-16 erg/s/cm2
The main characteristics of the observations are as follows.
- The targets are prioritized as reported in the OBs. As sensitivity is a key parameter
for our science goals, it is more important to complete all observations for the
highest
priority targets (if observable) before starting the observations for the next
ones,
in order of priority.
- There is no priority among the OBs for a given target (but for a shorter OB for
BX455).
OBs are named after the targets and with \"-0\", \"-1\", \"-2\", etc. appended
for different OBs.
- The DITs for our exposures of our faint targets are 600s (300s in one OB only)
- The brightest spectral feature of the targets is H_alpha in emission;
the observed wavelength, integrated flux, and size of H_alpha are thus
given in the table above.
- We are using the 100mas scale, with field of view (FOV) of 3.2\"x3.2\".
The targets are sufficiently compact to allow for \"on-source dithering\":
each sequence specified in the
SINFONI_ifs_obs_GenericOffsets template consists of \"O O O O O O\"
made up of three \"AB cycles\", where \"A\" and \"B\" are the two main positions
along the SE - NW direction with nod throw of half the FOV (i.e. 1.5\" along
each of RA and DEC) and small jitters in each AB cycle of about one-tenth
the FOV to minimize the number of redundant positions.
With this pattern, any 2 subsequent exposures overlap over one quadrant -
this area is sufficiently large to encompass the emission for our compact
targets. Opposite quadrants serve for sky subtraction in a pairwise fashion.
We have already observed Q1623-BX502 and ID6 successfully following exactly
this
strategy during one of our previous GTO run.
For all the others, we have obtained seeing-limited mode data at the 250mas
and
these data also show that the source is compact enough for on-source dithering
at 100mas scale.
We would like to emphasize that we have observed all the targets previously
with SINFONI, and we therefore know that the strategy in the present OBs will
be successful and map optimally the target's emission.
We would also like to note that for some of the targets the only TTS available is
rather
faint. We are aware of the possible limitations this could have on the AO
performance. Our experience from the SINFONI GTO visitor runs using AO in both
NGS and LGS mode with TTSs of similar magnitudes and at comparable distances from
the science targets was successful and provided effective angular resolution of
0.1\" - 0.2\", which still meets our scientific requirements.
We are thus confident that these observations can be carried out, and if
the acquisition presents some difficulties, we would like to kindly ask
the observers to do their best, or to contact the P.I. if needed.
Remarks on the finding charts:
- Two finding charts are provided for each target/OB, following the instructions
for SINFONI.
(1) The first one (SINFONI_{sourcename}_fchart1*) have wider FOV; a large and
a small black square show regions 1' x 1' and 8\" x 8\" centered on the target;
the TTS is labeled \"R1\".
(2) The second one (SINFONI_{sourcename}_fchart2*) is zoomed in on the target,
with the large and small solid-line squares showing regions of 8\" x 8\" and
3.2\" x 3.2\" centered on the target.
Waiver Requests
Critical Observing Condition Constraints
Transparency constraints:
- For all OBs, CLEAR sky transparency conditions is acceptable, as specified
in the proposal.
Moon constraints:
- For the fainter targets (K20-ID6, BX376 and SA12-6339) moon illumination may be
critical between OH lines. The same is for the targets with faint TTS (V >~
16, SA12-8768, BX599)), so we have set the constraints for moon illumination and
moon distance to 0.7 and 50 degrees, respectively, following the recommendations
from the ESO SINFONI P2PP Web pages
(http://www.eso.org/observing/p2pp/SINFONI/SINFONI-P2PP.html#Requirements)
For the other targets, we relax the constraints to moon illumination and distance
1.0 and 30 degrees.
Seeing constraints:
- Seeing < 0.8\", as specified in the proposal."
Time-Critical Aspects
Special Execution Requirements
As we explain in the General Description, the targets are prioritized
and the observations of the higher priority targets should be completed, if the
target is observable, before starting on a new target.
We have also noted in the General Description that the TTS for some targets are
rather faint. While from our experience during previous SINFONI GTO runs
we are confident the observations can be carried out and meet our scientific
requirements, please do not hesitate to contact the PI in case of difficulties.
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 15:40:24 2009
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