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 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 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 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 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 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 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 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 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 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 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 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 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 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 POS TARG OUTSIDE OF APERTURE 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 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 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 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 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 "between" on Visit 02 has been changed to July 7 2021 - Sept 13 2021 in order to copensate for HST going offline. -285880145 ----- Attempting Submission 2 (Wed Sep 09 21:15:23 GMT 2020) ----- ----- Attempting Submission 3 (Tue Feb 09 00:21:58 GMT 2021) ----- ----- Attempting Submission 4 (Mon Mar 22 21:24:11 GMT 2021) ----- ----- Attempting Submission 5 (Tue Apr 06 22:28:24 GMT 2021) ----- ----- Attempting Submission 6 (Thu Apr 15 17:27:55 GMT 2021) ----- ----- Attempting Submission 7 (Thu Jul 01 20:20:44 GMT 2021) ----- position warning may be ignored because we are employing large ~2000 pixel dithers. flash warning may be ignored because we are purposefully probing multiple background levels. 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 is known to fluctuate 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 a 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 this cycle (28) we will swap out NGC-6791 for Omega Centauri. Switching to Omega Centauri will provide significantly more stars, particularly at the faint end, which will improve the CTE measurements. Each cluster will have long and short exposures taken. NGC-104 short exposures will have 0 and 12 e-/pixel post-flash and Omega Centauri will have 0 and 6 e-/pixel post-flash. The long exposure Omega Centauri images will be taken with 4,8, 12, and 17 e-/pixel post-flash. NGC-104 long exposures will use a variety of post-flash levels: 0, 6, 12, 18, 24, 33, 55, 91, and 116 e-/pixel. All observations use the F502N filter. 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 has normally been taken at two epochs each cycle, starting six months after the last. The first epoch is typically scheduled in January/February 2021, the second epoch in July/August 2021. However this cycle we will change the schedule to help improve and expedite the ongoing work of the pixel-based CTE correction. Rather than observe Omega Centauri and NGC-104 during Jan. - Feb. 2021 we will observe only Omega Centauri between 02 Nov. 2020 - 28 Feb. 2021. We no longer require that both pairs of Omega Centauri and 47 Tuc observations are taken within seven days from each other. Instead we will sample all of Omega Centauri before the end of January 2021 and follow the same "betweens" as previous cycles for the remaining 2 visits of NGC-104 (Jan. 1 2021 - Feb. 28 2021 & July. 1 2021 - August. 31 2021). We have set visit-level timing requirements accordingly. ------ 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 17-27 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 47-TUC J2000 STELLAR CLUSTER GLOBULAR CLUSTER J2000 1625170545734 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /private/var/folders/75/7d0q6hm577j83brzkykpts3h0002_1/T/OPVisit11438385918147942505.xml USE SAME GUIDE STAR THROUGHOUT VISIT. 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