FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browserVisit 04 failed and I submitted a HOPR and was approved a for a repeat under HOPR 928941936846697----- Attempting Submission 1 (Thu Jul 14 20:49:27 GMT 2022) -----
----- Attempting Submission 2 (Fri Jan 26 17:21:33 GMT 2024) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 3 (Thu Jun 27 19:57:30 GMT 2024) -----
----- Attempting Submission 4 (Mon Jul 29 15:43:31 GMT 2024) -----all error or warnings regaring flash level or the target being outside of the aperture is expected and can be ignored.WFC3 UVIS CTE Monitor (Star Cluster)This program is a recurring UVIS calibration monitor that will observe two
stellar clusters (Omega Centauri, and 47 Tuc) to measure the flux loss of point
sources as a function of detector row number due to degrading Charge Transfer
Efficiency (CTE). Because CTE fluctuates with characteristics such as source
flux and background level, this program is designed to take short and long
exposures, at various commanded post-flash levels with the F502N filter. We will
compare the results from these new observations with previous external CTE
calibration programs and update the aperture phometry-based CTE model.
Furthermore, ACS has an external CTE calibration program that observes NGC 104
at various post-flash levels that can also be used for direct comparison.
Lastly, these data will be used to help monitor/improve the empirical
pixel-based CTE correction (FLC/DRC).Using clusters to measure the UVIS CTE relies on image pairs that have a ~2000
pixel (~ 1 chip height) dither. Each field is first observed in UVIS2, and then
dithered in the y-direction by an 81.6-arcsecond step (UVIS pixel scale ~ 0.04
arcsec/pixel), and then an identical exposure of the same field is taken in
UVIS1. This allows a source that is near an amplifier in one chip (exposure) to
be further from an amplifier in the other chip (exposure) enabling an absolute
measure of the CTE. With varying field density, post flash, and exposure length,
we build and maintain a CTE model based on many parameters.
In the past, the external CTE monitor has observed globular cluster NGC 104
(47 Tuc), and open cluster NGC 6791. The sparseness of NGC 6791 compared to
47 Tuc was used to test the effects of self-shielding on CTE-induced flux
losses. However, the CTE trending between the two targets has not shown a
significant difference. Therefore, starting cycle 28 we have swapped out
NGC 6791 for Omega Centauri. Switching to Omega Centauri provides
significantly more stars, particularly at the faint end, which improves the
CTE measurements.
Each cluster will have long and short exposures taken. NGC 104
short exposures will have 12 e-/pixel post-flash (~12 e- total background)
and Omega Centauri will have 0 and 11 e-/pixel post-flash (~1 and 12 e- total background).
The long exposure Omega Centauri images will be taken with a 10, 15, 23, 44, 75 and,
98 e-/pixel post-flash (20, 25, 34, 56, 92, and 117 e- total background). NGC 104 long
exposures will use post-flash levels: 0, 18, 24, 33, 55, 91, and 116 e-/pixel. (1, 20, 25,
34, 56, 92, 117 e- total background). All observations use the F502N.
Because of the ~2000 pixel dither, any warnings about the target being outside of
the aperture can be ignored. Any warnings regarding post-flash may also be
ignored since we're trying to simulate background levels with low/high commanded
post-flashes.
------- Scheduling -------
The CTE long-term monitoring observations are taken at two epochs each cycle,
starting approximately six months after the previous cycle's epoch.
Starting this cycle (30), we have removed the timing requirements for visits 02 and 04.
Previously we grouped Visit02 with Visit01 within x-number of days and the same thing
for Visit04 with Visit03. Rather than apply a group-within timing link, we set unique betweens
for each visit to help ensure the monitor obtains observations roughly ~6 months between
epoch 1 (visits 01 & 02) and epoch 2 (visit 02 & 03), and to hopefully help get the observations
on the official schedule easier.
------ Calibration Justification -------
These data will be used to determine the evolution of CTE with epoch,
position on the detector, and flash-level (i.e. background). Varying the
background levels via post-flash will allow us to monitor the effects of
post-flash to mitigate CTE. Results will be compared to Cycles 17-29 CTE
measurements for WFC3/UVIS CCDs.
The analysis of the data will be used to continue calibrating a model of
CTE-induced losses in both FLT and DRZ UVIS images, with a precision of better
than 1% for stellar photometry and less than 5% for astrometric effects from
CTE-induced source centroid shifts. Additionally, all exposures taken in this
program will also be used to test and improve the pixel-basedUVIS CTE correction
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