The list of Investigators does not match the STScI records for this program. MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 MAXIMUM DURATION EXCEEDED FOR INTERNAL OR EARTH CALIB SU 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 First submission. 432170194 ----- Attempting Submission 1 (Mon Dec 13 19:00:35 GMT 2021) ----- 1) I added the Co-I since the cal program was created with only a PI. 2) Re: max duration for internal: I've modeled these exposures after the dark calibration program, hence they use just over 1800s in an orbit to get two 900s exposures. 3) Postflash is varied to accomplish calibration objecitve. Testing a New Method for Pinning Down CTE losses Understanding CTE losses in WFC3/UVIS has very much been a learning experience. Once it became clear that there were significant losses at the small-electron-packet end, we realized that we needed more than the strategy that had worked so well for ACS: namely, just measuring the trails found behind the warm pixels (WPs) in the calibration long darks. We devised a strategy that used a combination of short-darks and long-darks. The long-darks allowed us to know the true intensity of each warm pixel, and the short darks with variable background allowed us to measure electron-survival as a function of background. This new strategy has worked well, but there are not as many WPs in the short darks as we would like. We experient here with a different approach. We will take the standard 900s long darks with a variety of post-flash levels so that the relative losses-vs-background can be assessed. This approach is not as direct as the short-long approach, but it may provide more data and it is actually more in-line with what actually gets done for science. Also, this new approach provides a lot more WPs to study, which should give us much better resolution on losses as a function of background. The short-dark data taken in the previous calibration cycle has noisy trends for backgrounds between 20e and 100e. This program should remedy that significantly. The observing strategy here is pretty straightforward. We will take long 900s darks at a variety of background levels. The standard calibration programs take 900s darks with zero post-flash background and with 20e added postflash, so this program will supplement those levels with twenty 900s exposures with a wide variety of backgrounds. In the end, we will have long darks with 22 different background levels: (0e), 4e, 8e, 12e, 16e, (20e), 24e, 28e, 35e, 42e, 49e, 46e, 63e, 70e, 77e, 84e, 98e, 126e, 161e, 203e, 252e, and 322e. The reduction plans are straightforward. The routine calibrations will give us around 20x900s darks with PF=20e from the same anneal period of this program. We will stack these images and make a list of the stable WPs. We will next select (say) WPs with between 45e and 55e found in the top ~250 pixels of the detector (i.e., the ones that suffer more than 1750 parallel transfers from the readot register). We will then examine the number of electrons read out for these pixels for the 22 background levels explpored. We can do the same for fainter and brighter WPs. These plots should provide more resolution than we have previously had to explore details in the charge-transfer model. We can of course compare these curves against predictions of the pixel-based model. Jay Anderson has been working on CTE for over 10 years and designed the pixel-based correction. Benjamin Kuhn has been spear-heading the external CTE monitor programs for the last few years. 0 false false RESTRICTED /Users/jayander/Desktop/OP-cache/APT_CAL16861_INTCTE-v01.xml Timing link suitability includes constraints ([02 After 01 by at most 5.0 days]) The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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