The list of Investigators does not match the STScI records for this program. POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT 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 POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE 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 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 POS TARG OUTSIDE OF APERTURE NO ORIENT 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 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 POS TARG OUTSIDE OF APERTURE NO ORIENT 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 POS TARG OUTSIDE OF APERTURE 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 NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT 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 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 NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT 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 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 Cycle 32, WFC3/UVIS External CTE Monitor, Phase 2, CAL proposal, submission 1 -2058949897 ----- Attempting Submission 1 (Mon Aug 26 17:21:22 GMT 2024) ----- All of the errors/warnings are expected and can be ignored for this calibration program 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, and 55 e-/pixel. (1, 20, 25, 34, and 56 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 scheduling for this program has evolved over the years, but we continue to set unique BETWEENs for each of the four visits (which started in cycle 30 PID 17009). In the past, before Cycle 30, we had observed two targets roughly twice a year. The motivation was to test whether or not the stellar density affected the CTE measurement due to shielding. Now that we have seen that shielding does not have a measurable effect on the CTE measurement (WFC3 ISR 2021-09), we observe Omega Cen and NGC 104 at four unique epochs throughout the cycle with at least ~2 months in between each visit. We elect to observe Omega Cen three times and NGC 104 only once. The motivation for this is the same as described above for replacing NGC 6791. Omega Cen has a much more favorable stellar density that provides ~1000's of stars per flux bin rather than ~100's. The increase in the number of sources (especially at the faint and bright ends) greatly reduced the uncertainty in the measurement. In this Cycle 32 proposal we will observe: Omega Cen - Visit01 ~ March 2025 NGC 104 - Visit02 ~ May 2025 Omega Cen - Visit03 ~ July 2025 Omega Cen - Visit04 ~ Dec 2025 - Jan 2026 ------ 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 17-31 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 algorithm developed by J. Anderson. 0 false false RESTRICTED STELLAR CLUSTER GLOBULAR CLUSTER J2000 STELLAR CLUSTER GLOBULAR CLUSTER 47-TUC J2000 The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. USE SAME GUIDE STAR THROUGHOUT VISIT. USE SAME ORIENTATION THROUGHOUT VISIT. 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CASM was run in Phase II mode. USE SAME GUIDE STAR THROUGHOUT VISIT. USE SAME ORIENTATION THROUGHOUT VISIT. (Tic-Visit :proposal-id 17674 :visit-id "03" :proposal-version -1 :trans-version "20240604" :date "15-Aug-2024 13:47:14.0" :trans-errors '(:WARNINGS 12 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17674 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17674 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2208 :al-overhead-at-end 69 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3062 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17674 :visit-id "03" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2152 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3062 :pcs-gap 0 ) false 2 0 The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. USE SAME GUIDE STAR THROUGHOUT VISIT. USE SAME ORIENTATION THROUGHOUT VISIT. (Tic-Visit :proposal-id 17674 :visit-id "04" :proposal-version -1 :trans-version "20240604" :date "15-Aug-2024 13:47:17.0" :trans-errors '(:WARNINGS 12 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17674 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17674 :visit-id "04" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2208 :al-overhead-at-end 69 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3062 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17674 :visit-id "04" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2152 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3062 :pcs-gap 0 ) true 2 0