Probing Red Supergiant Mass Loss 100-200 Years Before Explosion using UV Spectra of the Extraordinary SN 2023ixf

0 Assigned ID: 5807 ----- Attempting Submission 1 (Tue Mar 26 23:10:09 GMT 2024) ----- HST Phase I Proposal 5807 successfully submitted. Receipt: # 5807-1 ----- Attempting Submission 2 (Tue Mar 26 23:17:11 GMT 2024) ----- COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE Changed aperture in first visit to 52x0.5 to account for maximum drift during observation with a single guide star 524904157 ----- Attempting Submission 1 (Wed Aug 14 22:40:01 GMT 2024) ----- ----- Attempting Submission 2 (Fri Oct 25 00:06:27 GMT 2024) ----- ----- Attempting Submission 3 (Mon Dec 02 17:10:08 GMT 2024) ----- We arent using a small aperture and the coordinates are ICRS Probing Red Supergiant Mass Loss 100-200 Years Before Explosion using UV Spectra of the Extraordinary SN 2023ixf Mass loss in red supergiants is currently a topic of much debate, with proposed rates between 10^-7 and 10^-1 solar masses per year and hints of periods of enhanced mass loss which may be more prevalent as the red supergiant approaches explosion. However, observations of red supergiants tend to probe thousand of years prior to explosion while optical observations of the supernova probe the final 5 years and are only sensitive to the highest levels of mass loss. About 50 days after explosion, Lyman-alpha and Mg II emission lines form when there is interaction between the supernova ejecta and circumstellar medium, even when the optical is indistinguishable from a non-interacting supernova. These lines are extremely sensitive to all levels of circumstellar interaction, however, as the UV is very faint, obtaining these observations requires a very nearby supernova. On May 19, 2023, SN 2023ixf was discovered at 6.9 Mpc. Early spectra showed narrow, high-ionization emission lines characteristic of dense, confined circumstellar material which disappeared within a week. With a non-detection less than 24 hours before and rapid classification, this very nearby supernova was observed in exquisite detail from gamma rays to radio, including with HST in the UV starting just 3.5d after explosion and continuing through ~300d after explosion. With these observations, we can map out the mass-loss history of the red supergiant progenitor out to 75 years before explosion. Here, we ask for two epochs of FUV and NUV spectra, taking our mass-loss history of the progenitor star to ~200 years before explosion, giving us an unprecedented and detailed view of mass loss in a red supergiant. This program is to observe SN 2023ixf in the FUV and NUV at two epochs. The first epoch is 3 orbits (1 FUV, 2 NUV) and will be scheduled as a single visit before Mar 1, 2025. The faintest SN 2023ixf will be at this phase is V=21.5 The epoch will be broken into a FUV visit (2 orbits) and an NUV visit (5 orbits) scheduled within a week of each other. This epoch will occur after Mar 1, 2025 and after visit 1 by 4 months. The faintest SN 2023ixf will be at this phase is V=23 The Distance less than 40 Mpc team has extensive experience with UV observations and analyzing CSM interaction in hydrogen-rich supernovae at early and late times. We are members of the Global Supernova Project which has access to robotic telescopes for imaging and spectroscopy around the world and routinely PI programs for late time spectra on Keck, MMT, and the Large Binocular Telescope. K. A. Bostroem is a former member of the STIS team at STScI and has extensive experience with the STIS, Swift, Gemini, and Keck data reduction. Her research focuses on understanding the progenitors of hydrogen-rich CC SNe. She is the PI of programs to obtain HST/STIS UV data SN2022acko and SN2023ixf and already published a paper on Early CSM interaction in the optical spectra of SN 2023ixf. S. Valenti is the PI of a Cycle 31 program and a DD program to obtain HST/STIS FUV and NUV spectra of SN 2023ixf. He is the co-PI of DLT40. He has worked comprehensively on core collapse supernovae (CC SNe). M. Lundquist is an active member of the DLT40 team and specializes in the reduction and analysis of Gemini and Keck observations. He is currently a staff astronomer at the W. M. Keck Observatory. Prior to joining the DLT40 team, he worked as a Gemini Science Fellow at the Gemini Observatories. J. Andrews is an active member of the DLT40 team, has expertise observing with HST/STIS, and is an assistant astronomer at the Gemini Observatory. Her research focuses on characterizing the progenitors of core collapse (CC) SNe, specifically focusing on their mass-loss history via circumstellar interaction. D. Sand is the co-PI of the DLT40 survey and an expert in the progenitors of Type Ia SNe and SN environments. He has extensive experience with Swift, and Gemini observations of SNe and their environments. M. Shrestha is a Postdoctoral Research Associate at the University of Arizona. Her research focuses on the transients such as long gamma-ray bursts, core collapse (CC) SNe, and kilonova. She is part of DLT40 and SAGUARO collaborations. J. Jencson is an active member of the DLT40 team and has extensive experience in reducing and analyzing Swift observations of transients. His research focuses on multi-wavelength studies of hydrogen-rich transients and searches for dust-obscured transients and faint/failed SNe. G. Hosseinzadeh is an expert in early SN~Ia light curves and has experience analyzing early UV data. J. Pearson is focusing her thesis research on understanding the progenitors and environments of CC SNe and is an active member of the DLT40 team. Y. Dong is an senior graduate student in the DLT40 team and has experience analyzing both CC~SNe and SN~I. N. Meza is a graduate student in the DLT40 team focusing his thesis work on CC~SNe. E. Hoang is a graduate student in the DLT40 team focusing on stripped-envelope SNe. D. Janzen is a member of the SkyNet team which is responsible for maintaining the telescopes that the DLT40 team uses for their search. S. Jha is an expert in Type Ia supernovae and the PI of a program on SALT to obtain spectra of supernova transients. SALT is ideally located for obtaining rapid classification spectra of supernovae discovered by our Australian telescope. A. P. Ravi is a postdoc in the DLT40 team and has expertise in high energy emission from supernovae. He leads the UC Davis NIR observing program. D. Mehta is a graduate student in the DLT40 team focusing on short plateau SNe. 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