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 Resubmission with updates to use correct number of orbits. Added new Co-I as well. 94553400 ----- Attempting Submission 2 (Wed Apr 16 19:56:04 GMT 2025) ----- Flash levels are as expected. Added a new Co-I. The GS ACQ SCENARIO warning is puzzling us as we don't have any special requirments set at this time. WFC3 Astrometric Scale Monitoring The standard astrometric catalog in the field of globular cluster Omega Cen has been used to examine the geometric distortion of WFC3 UVIS and IR as function of wavelength in multi-cycle calibration programs over last 11 years of WFC3 on HST board. All observations from these programs have been reduced and provided the multi-wavelength geometric distortion in UVIS and IR detector. The derived geometric distortion coefficients implemented in the IDCTAB format are used in the HST pipe-line to correct for a ~7% distortion in WFC3/UVIS and IR images down to <1%. Additional to multi-wavelength WFC3 geometric distortion, all observations of Omega Cen taken through F606W and F160W UVIS and IR filters, respectively, during the last 11 years (all together 12 epochs) were used to look for time dependency of UVIS and IR geometric distortion and the effect of the scale change due to the thermal breathing. The results of the stability WFC3 geometric distortion published in WFC3-ISR-2015-02 (Kozhurina-Platais & Anderson, 2015), WFC3-ISR-2019-09 (Martlin, Kozhurina-Platais), have show that the UVIS geometric distortion is stable over 10 years on-orbit within 0.05 pixels or 2 mas in UVIS. The results of WFC3/IR published in WFC3-ISR-09-19 (M. McKay, Kozhurina-Platais, et al) have show that the IR geometric distortion is stable over 10 years on orbits within 0.1 pixel or 2 mas. The same observations were used to examine the WFC3/UVIS and IR photometric changes with time (WFC3-ISR-2020-05, Kozhurina-Platais, Bagget). The purpose of this calibration proposal is to continue the monitor of the stability of the WFC3 geometric distortion over time. The observations of Omega Cen through the UVIS F606W filter and the F160W IR filter will be used to derive the skew and scale terms of the geometric distortion and look for any secular changes over time. In addition, several UVIS and IR filters have been appended for the purposes of generating new PSF models for the community. The observation of Omega Cen through F606W and F160W is used as a standard filter in UVIS and IR, respectively. They are observed with the same pointing but with different roll-angle of the OTA at a single epoch between Jan -April 2026 at an orient of ~290 degrees. The 3 exposures in UVIS have steps of roll-angles -1.5, 0, +1.5 degrees requiring 3 orbits. The same 3 exposures in IR with the steps of roll-angles -1.5, 0, +1.5 degrees also require 3 orbits. To maintain accurate pointing control, 2-guide star acquisitions are used. If suitable guide stars can be found, the same pair of guide stars are used for all exposures. This cycle, additional filters are added for UVIS and IR for the purposes of building additional PSF models, based on usage statistics in GO science programs. ---Calibration Goals--- The geometric distortion of WFC3 in 13 UVIS and 8 IR filters were calibrated using the standard astrometric catalog of Omega Cen (Anderson & van der Marel, 2010). An update set of updated distortions were obtained for 20 UVIS filters using the same standard astrometric catalog of Omega Cen (Kozhurina-Platais, WFC3-ISR-2014-12; Martlin et al. WFC3-ISR-2018-11). The goal of this proposal is to monitor the geometric distortion of both the UVIS and IR detectors. The skew parameter in the ACS/WFC case, is changing with time in the level of 40 mas over 15 years on board of HST. The skew parameter is the non-perpendicularity of coordinate axes and is the major parameter in the geometric distortion model. 0 false false RESTRICTED CALIBRATION ASTROMETRIC SPATIAL DISTORTION TEST This is the same target (and coordinates) as used in CAL/WFC3 11911, UVIS L-Flats and Geometric Distortion and in other multi-cycles calibration proposals J2000 /private/var/folders/z3/xy_g1v_s5fz9yrhzb8thz4cr0001qc/T/OPVisit10897430132948648585.xml The scheduling data was generated by CASM 33.0. CASM was run in Phase II mode. 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