Upated Special Requirements to include BETWEEN values from APT. -1591133344 Assigned ID: 6997 ----- Attempting Submission 1 (Fri Apr 10 17:59:10 GMT 2026) ----- HST Phase I Proposal 6997 successfully submitted. Receipt: # 6997-1 ----- Attempting Submission 2 (Mon Apr 13 14:43:35 GMT 2026) ----- Updated Orbits 2 and 3 to have exp time <1000s I don't think I have more than 6 orbits according to APT, but not sure how to figure this out otherwise. 88335218 ----- Attempting Submission 1 (Wed May 13 21:53:48 GMT 2026) ----- HST Phase II Proposal 18250 successfully submitted. Receipt: # 18250-1 ----- Attempting Submission 2 (Thu May 14 01:29:41 GMT 2026) ----- HST Phase II Proposal 18250 successfully submitted. Receipt: # 18250-2 ----- Attempting Submission 3 (Thu May 14 01:42:44 GMT 2026) ----- HST Phase II Proposal 18250 successfully submitted. Receipt: # 18250-3 ----- Attempting Submission 5 (Fri May 15 19:22:00 GMT 2026) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 6 (Tue May 19 16:08:06 GMT 2026) ----- HST Phase II Proposal 18250 successfully submitted. Receipt: # 18250-6 ----- Attempting Submission 7 (Tue May 19 20:22:22 GMT 2026) ----- There is a deepening body of literature demonstrating that M dwarfs flare at ultraviolet, optical, and infrared wavelengths throughout their lifetimes. At the same time, M dwarf flares inhibit our interpretation of planetary transmission spectra. No exoplanet system demonstrates this fact better than TRAPPIST-1, where transmission spectra of rocky planets are rife with stellar contamination. Rather than dwell on stellar contamination as a problem, here we propose use it to uncover the time-dependent and panchromatic nature of low-mass stellar flares. To do so we propose to align HST with already approved JWST multi-cycle Program 6456/9256 to capture a TRAPPIST-1 flare simultaneously in the far ultraviolet (FUV) and near infrared (NIR). Given the stringent time constraints of the accepted JWST program, this is a golden opportunity to unlock flare behavior over time and at two anchor points across the electromagnetic spectrum. The only opportunity to make these observations is rapidly approaching and we require the DD option to make this critical link between M dwarf flares in the FUV and NIR. We are requesting 6 HST/COS orbits to connect the FUV and NIR behavior of a TRAPPIST-1 flare. We will observe TRAPPIST-1 for 6 orbits using COS/G130M/1222A simultaneously with the Obs 13 of JWST GO 9256. Dr. Hannah Diamond-Lowe has previously PI'd HST programs and led work on the characterization of M dwars in the UV, which has included flare detection and analysis. Natalie Allen is an expert on the observation and interpretation of exoplanet atmospheres, and on the characterization of stellar activity. She is the PI of JWST GO 6456/9256 to characterize TRAPPIST-1 e. Dr. Nestor Espinoza's expertise is on the interpretation and observation of exoplanet atmospheres, as well as JWST instrumentation and data analysis. Dr. Ward Howard (CU Boulder) is an expert in the multi-wavelength properties of stellar flares and flare mitigation in transmission spectroscopy. He led the first analyses of IR flare spectra with JWST for K to M dwarfs including TRAPPIST-1, and is the PI of previously accepted multi-wavelength flare monitoring programs of other nearby M stars with Chandra, Swift, ALMA, TESS, and JWST. Dr. Meredith MacGregor is an expert at studying stellar flares at radio through X-ray wavelengths, including leading several HST programs targeting nearby M dwarfs such as Proxima Centauri and Wolf 359. Dr. Guadalupe Tovar Mendoza is an expert in M dwarf stellar flares, and has experience working with multi-wavelength flare observations. Exoplanets and Exoplanet Formation Stellar Physics and Stellar Types 0 Discovery false false SUPPORTED STAR BROWN DWARF NO Updated by PI from Gaia DR3. J2000 J2000 STAR K V-IV NO Updated by PI from Gaia DR3. J2000 COS/FUV Spectroscopic No No G130M 1222 1779223195495 /System/Volumes/Data/solaris/user1/williamj/hst/work/cycle33/OP-cache/18250-v01.xml The scheduling data was generated by CASM 34.1. CASM was run in Phase II mode. 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