2025-04-22 |
hst_1229.pmap |
archived |
These WFC3 UVIS superdarks will affect all UVIS data taken from February 25, 2025 to March 30, 2025. Currently, the automated calibration pipeline and CRDS have only WFC3 UVIS drk and dkc reference files with USEAFTER dates of up to February 22, 2025. The automated pipeline should now use these reference files to perform dark subtraction on any UVIS datasets obtained between the dates above, as they represent the most accurate picture of dark current and hot pixels for this time period. These WFC3 UVIS drk and dkc files were generated using dark exposures from HST Cycle 32 CAL programs 17665, 17667, and 17668. More information regarding the method used to create the UVIS dark calibration reference files can be found in WFC3 ISR 2016-08. Additionally, the header of each reference file contains a detailed history section outlining the process, and provides a list of data used to create each file.
These two new bad pixel tables with USEAFTERs of February 25, 2025 and March 29, 2025, were generated using data taken from February 26 through March 27, 2025 and March 29 through April 3, 2025. Currently, the Calibration Reference Data System only has WFC3 UVIS bad pixel reference tables up to a USEAFTER date of January 28, 2025. The automated pipeline should now use these reference file as the bad pixel table on any UVIS datasets obtained between the dates above, or beyond because they represent the most accurate measure of pixel stability at the time of the science observation. These WFC3 UVIS bad pixel files were generated using 900 second dark exposures from the HST cycle 32 daily monitoring programs 17665, 17667, and 17668. More information about the UVIS bad pixel tables is outlined in the WFC3 ISR 2018.15 and WFC3 ISR 2021.14. |