The list of Investigators does not match the STScI records for this program. SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE This is the standard HST focus monitor program. 253191823 ----- Attempting Submission 1 (Thu Nov 10 04:25:27 GMT 2022) ----- Isabel Rivera, a member of the WFC3 team, should be added as a coI. The other errors and warnings are the usual ones for this program. HST Cycle 30 Focus & Optical Monitor Utilize WFC3/UVIS and ACS/WFC in parallel to observe stellar cluster members with multiple exposures over an orbit. Phase retrieval performed on the PSF in each image will be used to measure focus, with the ability to explore apparent coma, astigmatism, and third order spherical changes in WFC3. The goals are to 1) monitor the optical telescope assembly focal length for the purposes of maintaining focus within science tolerances and 2) determine focus offsets between the imagers and identify any science instrument-specific focus behavior and dependencies. For Cycle 30, we convert the standard CAL/OTA monitor to a CAL/WFC3 monitor. This bi-monthly program uses the WFC3/UVIS filter F410M to take shallow subarray exposures of the sparse open cluster NGC188. Full frame ACS/WFC exposures in filter F502N are made in parallel. Phase retrieval (PR) is performed on the stellar images to measure the focus of each exposure in equivalent secondary mirror despace. These focus measurements are used to track the evolution of the focus over months and years and to inform whether a focus adjustment is required. One orbit every ~2 months with WFC3/UVIS and ACS/WFC in parallel for con-focality check. The use of WFC3 subarrays allows for more exposures during the orbit. Since deployment, the HST OTA has shrunk by ~150 microns, resulting in over 20 compensating Secondary Mirror (SM) adjustments away from the Primary Mirror to maintain good focus to the science instruments. This program provides the observations to determine when an secondary mirror adjustment is required. 0 false false RESTRICTED STELLAR CLUSTER OPEN CLUSTER NO magnitude not relevant J2000 /private/var/folders/dk/9vcy4n7569l7sc6lyj83l0f000037q/T/OPVisit11534669244110417609.xml The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 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