0 Assigned ID: 4313 ----- Attempting Submission 1 (Wed May 24 12:52:51 GMT 2023) ----- HST Phase I Proposal 4313 successfully submitted. Receipt: # 4313-1 ----- Attempting Submission 2 (Wed May 24 19:45:57 GMT 2023) ----- Made a copy of target 1; changed the central co-ordinates slightly to get the appropriate FOV for visit 51, which has May 06 to 30, 2024 plan window ; the new target 2 is CYGLOOP-SE-CLOUD-TWEAK. -888689104 ----- Attempting Submission 1 (Thu Sep 07 20:36:02 GMT 2023) ----- ----- Attempting Submission 2 (Mon Apr 22 16:35:00 GMT 2024) ----- Evolution of an isolated shock-cloud interaction along the southeastern boundary of the Cygnus Loop supernova remnant We propose to use WFC3 narrowband imaging to obtain HST 2nd epoch H-alpha, [S II] and [O III] images of an isolated shock-cloud interaction in the Cygnus Loop that was previously observed in 1994 using WFPC2. The two sets of images separated by over 30 years will allow us to characterize the evolution of the shocked gas in great detail. Proper motions will be measured to an accuracy of better than 1.5 mas/yr. Thus, for well defined filaments and knots, the shock velocities will be determined based on the accurate GAIA-derived distance to the Cygnus Loop (725 +/- 15 pc) to within about 5 km/s. The differences in shock velocities along a filament and at different locations will allow us to estimate the variation in the pre-shock densities that exist within the cloud. Instabilities and shearing in the flow, or the development of turbulence will be seen as changes in the emission morphologies. The brightening of [O III] and [S II] emission relative to H-alpha will indicate that the recombination zone behind the shock front is getting stronger, and conversely the morphologies and brightnesses will remain more or less the same if the shock-front is moving in steady state. The long temporal baseline between observations combined with the high angular resolution of the HST instruments provides a powerful tool for analyzing the various physical processes that drive supernova remnant shock-cloud interactions. Three WFC3/UVIS filters, F656N, F673N and F502N will be used to image a single field in the Cygnus Loop supernova remnant in H-alpha, [S II] and [O III], respectively. The region to be observed is a shock-cloud interaction along the south-east perimeter of the remnant that has been imaged previously by WFPC2. We require all the exposures to be at the same orientation, and have specified them in a single four-orbit visit. For each exposure a standard dither pattern to cover the chip gap plus a sub-pattern to remove cosmic rays and bad pixels have been specified. We have also included a FLASH for each sub-exposure, as recommended. Although the region of interest will be covered at any orientation, there are features near the edges of the field that are critical to include that may require the co-ordinates to be tweaked after the visits have been scheduled in the long-range plan. Once the target is scheduled we request the opportunity to update the target co-ordinates in the Phase II proposal before the visit executes. Drs. Blair, Raymond, and Sankrit have been co-authors on several papers on the Cygnus Loop supernova remnant. All three co-investigators are experienced in the use of HST for the study of supernova remnants. Dr. Raymond is a world-acknowledged expert on shock astrophysics. Dr. Revalski is an expert in the reduction, custom-calibration, and drizzling of HST WFC3 imaging, as well as precision astrometry, PSF modeling, and photometry. Stellar Physics and Stellar Types Stellar Populations and the Interstellar Medium 6 false false false false false false false false SUPPORTED ISM EMISSION LINE NEBULA SHOCK FRONT SNR J2000 J2000 H-alpha surface brightness 6.0 +/- 0.5 E-15 erg/s/cm2/arcsec2 ISM EMISSION LINE NEBULA SHOCK FRONT SNR J2000 J2000 H-alpha surface brightness 6.0 +/- 0.5 E-15 erg/s/cm2/arcsec2 WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F673N POS-TARG MOSAIC DITHER 3 2.414 WFC3-UVIS-DITHER-LINE-3PT false true 1.485 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 46.84 1 true The scheduling data was generated by CASM 32.0. 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