Start Date | Context | Status | Description |
---|---|---|---|
2025-02-17 | hst_1212.pmap | latest | The ACS WFC bias, dark, CTE dark, and sink files were generated following the ACS WFC anneal on February 11, 2025, and should be used to calibrate ACS WFC observations taken between January 18, 2024 and February 11, 2025. |
2025-02-05 | hst_1211.pmap | archived | This new bad pixel table with USEAFTER of January 4, 2025 was generated using data taken from January 5, 2025, through January 27, 2025. Currently, the Calibration Reference Data System only has WFC3 UVIS bad pixel reference tables up to a USEAFTER date of December 3, 2024. The automated pipeline should now use this reference file as the bad pixel table on any UVIS datasets obtained between the dates above, or beyond because it represents 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 and 17667. More information about the UVIS bad pixel tables is outlined in the WFC3 ISR 2018.15 and WFC3 ISR 2021.14. These WFC3 UVIS superdarks will affect all UVIS data taken from January 4, 2025 to January 25, 2025. Currently, the automated calibration pipeline and CRDS have only WFC3 UVIS drk and dkc reference files with USEAFTER dates of up to January 1, 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 and 17667. 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. |
2025-02-03 | hst_1209.pmap | archived | Since 2019, IR bad pixel tables and superdarks incorporate a new time dependence characteristic to the pixel quality for better calibration and flagging and tracking bad pixel behavior. These behaviors include hot and unstable pixels and whether any bad pixel has regained its stability since launch. One new bad pixel table is present for data obtained through Cycle 31 with a USEAFTER date of December 22, 2023. Since launch, a litany of circular aberrant regions called blobs have appeared in IR images. These blobs are regions of lower sensitivity that appear due to bits of epoxy from the CSM motor shafts depositing onto the mirror. Tracking and flagging these blobs in the IR bad pixel table is therefore imperative so that they may be masked in any science images where they may appear. Information regarding blobs can be found in WFC3 ISR 2018 06. The two most recent blobs appeared on MJD 59378 and 59860, which are corrected in the previous IR bad pixel table. This table presents no new IR blobs that were not already corrected for in previous IR bad pixel tables. |
2025-01-27 | hst_1208.pmap | archived | Delivery of new STIS CCD bias and dark reference files for CCD data taken between December 26, 2024 and January 22, 2025. The files were generated from data taken in the same time frame under STIS calibration programs 17632 and 17629. |