This resubmission includes modifications to visits W4 and H4 to
test for changes in the 47 Tuc photometry caused by switching to the
Side2 electronics. We cycle through all CCD filters and perform an
additional gain test. Two additional external orbits are required.
----- Submission 1 (Fri Sep 02 20:07:55 GMT 2005) -----
----- Submission 2 (Thu Jun 22 20:47:07 GMT 2006) -----
CCD Stability Monitor
This program will verify that the low frequency flat fielding, the
photometry, and the geometric distortion are stable in time and
across the field of view of the CCD detectors. A moderately crowded
stellar field in the cluster 47 Tuc is observed every three months with
the HRC (at the cluster core) and WFC (6' West of the cluster core) using
the full suite of broad and narrow band imaging filters. The positions
and magnitudes of objects will be used to monitor local and large scale
variations in the plate scale and the sensitivity of the detectors and
to derive an independent measure of the detector CTE. An additional orbit
is required to compare WFC observations taken at gain 1 with those taken
at the new default gain 2.
The total number of orbits for both detectors is 13 orbits.
HRC: 1 orbit every 3 months for a total of 4 orbits.
WFC: 2 orbits every 3 months for a total of 8 orbits.
1 additonal orbit to evaluate the relative gain ratios.
For the HRC and WFC detectors, all filters are tested every visit, with the
exception of the F658N and F660N which are tested alternatively.
HRC: Orbit#1) 01=F435W 02=F475W 03=F555W 04=F606W 05=F625W 06=F775W 07=F814W
08=F850LP 09=F344N 10=F502N 11=F892N 12=F550M 13=F660N, F658N alternately
WFC: Orbit#1) 01=F435W 02=F555W 03=F625W 04=F814W 05=F475W 06=F550M
Orbit#2) 01=F606W 02=F775W 03=F850L 04=F502N 05=F892N 06=F660N, F658N alternately
Updates to the relative sensitivity as a function of position on the
detector will be provided via updated flat field reference files. Any
changes in absolute sensitivity of the detectors as a function of time
will be used to update the CCD QE curves used by the pipeline. The relative
gain ratios will be used to verify the values in the CCD parameters table.
Variations with respect to the previous observations will allow us to create flats
accurate to 1% over the detector field of view. No absolute photometric
calibration is provided by this program. Updates to the geometric distortion
coefficients will also be provided.
Observations of 47 Tuc using the HRC & SBC UV filters will be obtained in
the UV contamination monitor program (10736).
12
false
0.0
false
false
false
false
false
RESTRICTED
STELLAR CLUSTER
GLOBULAR CLUSTER
Magnitude of main-sequence turn-off stars.
Field at cluster centre.
J2000
00 00 0.0000
+00 00 0.00
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
Magnitude of main-sequence turn-off stars.
Field 6' W of cluster centre.
J2000
00 00 0.0000
+00 00 0.00
J2000
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