0 Assigned ID: 6931 ----- Attempting Submission 1 (Thu Oct 23 04:24:44 GMT 2025) ----- HST Phase I Proposal 6931 successfully submitted. Receipt: # 6931-1 ----- Attempting Submission 2 (Thu Oct 23 16:18:51 GMT 2025) ----- HST Phase I Proposal 6931 successfully submitted. Receipt: # 6931-2 0 ----- Attempting Submission 1 (Mon Nov 03 16:49:44 GMT 2025) ----- HST Phase II Proposal 18214 successfully submitted. Receipt: # 18214-1 ----- Attempting Submission 2 (Mon Nov 03 21:03:30 GMT 2025) ----- HST Phase II Proposal 18214 successfully submitted. Receipt: # 18214-2 ----- Attempting Submission 3 (Mon Nov 03 21:12:07 GMT 2025) ----- ----- Attempting Submission 4 (Tue Nov 04 06:54:36 GMT 2025) ----- ----- Attempting Submission 5 (Tue Nov 04 20:50:21 GMT 2025) ----- ----- Attempting Submission 6 (Tue Nov 04 22:38:05 GMT 2025) ----- HST Phase II Proposal 18214 successfully submitted. Receipt: # 18214-6 ----- Attempting Submission 7 (Tue Nov 04 23:21:13 GMT 2025) ----- Spectral Synergy of SN2023ixf: A unique insight into a nearby, radio- bright core-collapse supernovae. SN2023ixf has been one of the most studied core collapse supernova, although it has faded in the optical domain, the transient has become bright in the radio. A recent re-brightening event offers a unique opportunity to extend the multi-domain observations of this object in the optical and radio. There is a Rapid Response Time proposal was granted using eMERLIN VLBI to make a series of 5 observations, of which the first two have been completed with a clear detection of the order of 1 mJy. However, the insights provided by the UV and optical spectra will provide a detailed analysis of the CSM conditions and shockwave characteristics. HST remains the only instrument capable of providing the spectra for SN2023ixf at this late stage, as we require the UV, and M101 is a Spring target. The combination of data in these domains will provide a clear understanding of CSM properties at the current shockwave radius and a direct insight into the progenitor history. The interaction of the CSM properties and the shockwave, creating the synchrotron radio emission, will constrain the power law arguments related to CSM density changes with time and distance. In addition, provide a test for recent considerations of alternatives to CSM density as a the sole cause of deviation from power law models in the radio domain. This program is to observe SN 2023ixf from the optival to the FUV. The first epoch is 2 orbits, and will be scheduled as a single visit before Nov 8 2025. The subsequent epochs (also 2 orbits each), will repeat the same setup, with the second epoch taking place between 10-15 days after the 1st epoch. The 3rd epoch being 10-15 days after the 2nd epoch. However, if we do not see significant evolution, we will forego the third epoch, unless there is unexpected evolution in our radio observations. The faintest SN 2023ixf will be at this phase is V=23 mag. . PI: Dr Conor Ransome (Steward Observatory, University of Arizona), Postdoctoral Research Associate. CR has extensive experience in the photometric and spectroscopic follow-up of supernovae. His research focus is on supernovae that interact with surrounding material. He has experience with Fitting models to HST data of the progenitor of SN2023ixf. Diane Swan (University of Lancashire), PhD Student (year 1). DS is a part-time PhD student who is studying the interaction of radio-bright core-collapse supernovae with the surrounding CSM material. These data will be analyzed immediately and will produce a peer-reviewed publication lead by DS as well as contributing to her thesis. Dr Joanne Pledger (nee Bibby) (University of Lancashire), Reader in Astrophysics. JP has experience of planning photometric and spectroscopic Gemini/GMOS observations of Wolf-Rayet stars and has reduced and analyzed these data using tools described in the experimental design. JP has published work based on this data. She led the first paper on SN2023ixf, identifying the progenitor in HST imaging. Her research also focuses on investigating SN environments using spectroscopic data and identifying SN progenitors using archival data. Dr Megan Argo (University of Lancashire), Reader in Astrophysics. MA is the radio expert on the supervisory team and overseeing the supporting radio data is of sufficient quality before triggering the optical ToO. She is also part of the e-MERLIN legacy survey team. Stellar Physics and Stellar Types 0 false SUPPORTED STAR CIRCUMSTELLAR MATTER SUPERNOVA SUPERNOVA TYPE II NO This object was generated by the targetselector and retrieved from the NED database. J2000 J2000 EXT-STAR K V-IV g=20.48, r=20.43, z=20.39 J2000 STIS/CCD Spectroscopic No No G750M 6581 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750M 6581 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750M 6581 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 Timing link suitability includes constraints ([Group (01 02) Within 1.0 days]) The scheduling data was generated by CASM 33.1. 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