0 Assigned ID: 4836 ----- Attempting Submission 1 (Wed May 24 23:45:52 GMT 2023) ----- HST Phase I Proposal 4836 successfully submitted. Receipt: # 4836-1 ----- Attempting Submission 2 (Wed May 24 23:48:22 GMT 2023) ----- HST Phase I Proposal 4836 successfully submitted. Receipt: # 4836-2 Could not connect to APT Status Server fixing buffertime in last exposure of COS visit 229959635 ----- Attempting Submission 1 (Mon Sep 11 21:50:35 GMT 2023) ----- HST Phase II Proposal 17497 successfully submitted. Receipt: # 17497-1 ----- Attempting Submission 2 (Thu Sep 14 22:25:38 GMT 2023) ----- ----- Attempting Submission 3 (Thu Dec 07 19:58:29 GMT 2023) ----- ----- Attempting Submission 4 (Fri Dec 08 00:42:58 GMT 2023) ----- ----- Attempting Submission 5 (Fri Dec 08 16:45:16 GMT 2023) ----- the only change since the last submission is the buffertime of the last exposure UV CSM Interaction in the extremely nearby SN 2023ixf in M101 The 2023 May 19 explosion of SN2023ixf in the nearby (~6.4 Mpc) spiral galaxy M101 has presented us with a once in an HST-lifetime chance to get a comprehensive NUV to NIR dataset of an interacting core collapse supernova. This non-disruptive ToO will be complementary to two already approved Cycle 30 proposals which have been triggered on this object. We will observe SN~2023ixf between 100 and 200 days after explosion to constrain any CSM interaction with CSM interaction. Late UV observations are the best way to constrain interaction for typical RSG mass loss rates. With only a handful of core-collapse supernovae observed in the ultraviolet with HST, and almost all within 3 weeks of explosion, this proposal fills a crucial gap in our knowledge of the evolution of core-collapse supernovae in the ultraviolet. This can only be done with HST, and only with a SN that is this close can we probe the UV far into time periods when the flux has normally faded significantly. This proposal will be triggered on SN 2023ixf a nearby SN discovered on 19 May 2023. We will observe the SN with STIS FUV-MAMA G140L observation with the 52x0.2" slit and STIS NUV-MAMA G230L observation with the 52x0.2" slit. The observations will be triggered beween October and November 2023 in the first window of observation. The PCR 92628 for HST program 17497 has been appoved and this proposal can be triggered in cycle 30. S. Valenti is the PI of this proposal. He has worked comprehensively on core collapse supernovae (CC SNe). K. A. Bostroem extensive experience with the STIS data reduction and the reduction and analysis of core collapse supernovae observations with Swift and Gemini. Her research focuses on understanding the progenitors of hydrogen-rich CC SNe. 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. J. Andrews is an active member of the DLT40 team, has expertise observing with HST/STIS, and is an assistent astronomer 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. M. Lundquist is an active member of the DLT40 team and specializes in the reduction and analysis of Gemini and TESS observations supplementary to this proposal. 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. G. Hosseinzadeh is an expert in early SN~Ia light curves and has experience analyzing early UV data. J. Jencson is an active member of the DLT40 team and has extensive experience in reducing an 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. 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 active member of the DLT40 team and has experience analyzing both CC~SNe and SN~I. N. Meza is a member of the DLT40 team focusing his thesis work on CC~SNe. Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE II J2000 J2000 EXT-STAR SUPERNOVA TYPE II NO J2000 J2000 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 The scheduling data was generated by CASM 31.1. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 17497 :visit-id "02" :proposal-version -1 :trans-version "20230627" :date "05-Dec-2023 11:27:18.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 261408 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17497 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17497 :visit-id "02" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2483 :al-overhead-at-end 0 :internal-dur-at-end 113 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2926 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17497 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2534 :al-overhead-at-end 85 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2926 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17497 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2534 :al-overhead-at-end 85 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2926 :pcs-gap 0 ) false 3 0 The scheduling data was generated by CASM 31.1. 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