README web version of /home/usg/OPS/MTS/readme_xml/readme_80033900
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
Information on targets and AO TTS:
OB names R(NGS) target separation comments
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Q2346-BX482 15.4 K~21 50 arcsec H_alpha: line at 2.138um
integrated flux ~1.1e-16 erg/s/cm2
major axis FWHM ~ 1.5"
K20-ID6 ~16 K=19.9 55 arcsec H_alpha: line at 2.124um
integrated flux ~0.6e-16 erg/s/cm2
major axis FWHM ~ 1.0"
Q1623-BX502 15.5 K=21.8 8.5 arcsec H_alpha: line at 2.072um
integrated flux ~1.3e-16 erg/s/cm2
major axis FWHM ~ 0.4"
The main characteristics of the observations are as follows.
- The targets have the following priority:
beginning of P80: 1) Q2346-BX482 : 6 OBs
early-middle P80: 2) K20-ID6 : 6 OBs
end of P80 : 3) Q1623-BX502 : 2 OBs
- Sensitivity is a key parameter for our science goals. It is more important
to complete all observations for the highest priority target before starting
the observations for the next ones, in order of priority.
- There is no priority among the OBs for a given target. 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.
- 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".
Two different strategies are followed, depending on the target.
(1) Two of our targets (K20-ID6 and Q1623-BX502) 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. This is indicated
in the finding charts (described below).
With this pattern, any 2 subsequent exposures overlap over one quadrant -
this area is sufficiently large to encompass the emission for our two compact
targets. Opposite quadrants serve for sky subtraction in a pairwise fashion.
We have already observed Q1623-BX502 successfully following exactly this
strategy during one of our previous GTO run.
For K20-ID6, 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.
(2) The third target, Q2346-BX482, is significantly more extended based on our
previous seeing-limited mode data, and proper full coverage of the entire
source requires in this case to offset to sky positions away from the source.
The sequence is here "O S O O S O", where each "O" on-source pointings is
offset by approximately 0.2" along RA and DEC in four positions around the
target (in analogy to imaging, this corresponds to a jitter box width of
0.4", except the jitters are not random). Again, this is indicated in the
finding charts (see below).
We would like to emphasize that we have observed all three 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 K20-ID6, 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.
In addition, for K20-ID6 and Q1623-BX502, two dashed-line squares show
the two main dithering positions of the sequence, where the source lies
in opposite quadrants for any two successive exposures (explained above).
For Q2346-BX482, its size prevents such on-source dithering and the
dashed squares indicates the full region mapped accounting for the
small offsets between the 4 on-source exposures (explained above).
Waiver Requests
Two Waiver Requests were submitted:
080.A-0339A.01.WAV: for an extension of P2PP submission dealine until October 10
(submitted on August 01, 2007; Approved on August 02, 2007)
080.A-0339A.02.WAV: for an increase of the OB execution time limit to 1h40.
(submitted on October 05, 2007; Approved on October 05, 2007)
Critical Observing Condition Constraints
Transparency constraints:
- For all OBs, CLEAR sky transparency conditions is acceptable, as specified
in the proposal.
Moon constraints:
- For all targets, conforming to our proposal, there is no constraint on
lunar phase and so the illumination is set to 1.0.
- For K20-ID6, the TTS is faint (V >~ 16), however, so we have set the
constraint for moon distance to 50 degrees
(following recommendations from the ESO SINFONI P2PP Web pages
(http://www.eso.org/observing/p2pp/SINFONI/SINFONI-P2PP.html#Requirements)
- For the other two targets, we relax the constraints to moon distance of
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
before starting on a new target.
Priorities are as follows:
beginning of P80: 1) Q2346-BX482 : 6 OBs
early-middle P80: 2) K20-ID6 : 6 OBs
end of P80 : 3) Q1623-BX502 : 2 OBs
We have also noted in the General Description that the TTS for K20-ID6
is 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 15:40:21 2009
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