0 Assigned ID: 5804 ----- Attempting Submission 1 (Tue Mar 26 23:09:06 GMT 2024) ----- HST Phase I Proposal 5804 successfully submitted. Receipt: # 5804-1 ----- Attempting Submission 2 (Tue Mar 26 23:48:03 GMT 2024) ----- HST Phase I Proposal 5804 successfully submitted. Receipt: # 5804-2 ----- Attempting Submission 3 (Wed Mar 27 00:00:26 GMT 2024) ----- HST Phase I Proposal 5804 successfully submitted. Receipt: # 5804-3 ----- Attempting Submission 4 (Wed Mar 27 00:04:50 GMT 2024) ----- Resubmissing Phase II for review, but with F336W has cosmic split. -756218895 ----- Attempting Submission 3 (Mon Jul 22 02:14:33 GMT 2024) ----- HST Phase II Proposal 17777 successfully submitted. Receipt: # 17777-3 ----- Attempting Submission 4 (Tue Jul 23 22:23:59 GMT 2024) ----- HST Phase II Proposal 17777 successfully submitted. Receipt: # 17777-4 ----- Attempting Submission 5 (Mon Aug 05 21:26:39 GMT 2024) ----- ----- Attempting Submission 6 (Thu Mar 12 21:23:08 GMT 2026) ----- ----- Attempting Submission 7 (Mon Mar 16 17:30:15 GMT 2026) ----- Confirming the first progenitor candidate of a rare type Ibn supernova Type Ibn supernovae (SN Ibn) are hydrogen-poor SNe that interact with their hydrogen-poor circumstellar medium (CSM). They probe the advanced and little-understood stage of mass loss that strips helium from a massive star. SN 2023fyq is the closest SN Ibn to date at 18.2 Mpc. The explosion site of SN 2023fyq was imaged with HST in several filters (UV through NIR) 12 years before explosion, revealing a blue (B - V = 0.2) and luminous point source with M = -9.5 mag, consistent with either a WC/O-type star or a young cluster with a turnoff mass of >20 Msun. We propose to obtain 4 orbits of deep HST imaging approximately two years after explosion to confirm the progenitor of SN 2023fyq and to discern its cluster or single stellar system nature -- yielding the first progenitor identification for a SN Ibn. Such a discovery would be crucial to understanding the mass loss mechanism responsible for stripping 1/3 of all core-collapse supernova progenitors of their hydrogen and/or helium, and to understanding what a stripped star looks like before its explosion. We request 4 orbits of HST imaging in Cycle 32 to observe SN 2023fyq in 5 filters, 2 years after explosion. There filters will achieve a depth of ~26 mag (M=-6), and will allow us to confirm that the progentor candidate for SN 2023fyq.s Dr. Kirsty Taggart is an observer focused on the host galaxies of core-collapse supernovae. Dr. Kaew Tinyanont has a previously approved JWST program for SN 2014C. He is an expert on NIR photometry, spectroscopy, and dust modelling of core-collapse supernovae. Kyle Davis is a graduate student working on supernova spectroscopy and focusing on infrared observations. They have previously worked on a Icn supernova project, and are studying the NIR and MIR properties of interacting SNe as part of their PhD. Dr. Ryan Foley is an expert transient observer. He has preferred access to telescopes at Lick and Keck Observatory. He is PI of the Keck Infrared Transient Survey, a NASA Key Strategic Mission Support program to obtain NIR spectra of astrophysical transients. Stellar Physics and Stellar Types 6 false false false false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE IB NO J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/IR Imaging No No F160W POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 3 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 4 false Timing link suitability includes constraints ([02 After 01 by at most 14.0 days]) The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. Estimates magnitudes (all AB mag): - WFC3_UVIS1/F336W 26.28 - WFC3_UVIS1/F438W 26.28 - WFC3_UVIS1/F814W 26.20 - WFC3_UVIS1/F606W 26.05 For SNR 8: F336W = 1,756 s - https://etc.stsci.edu/etc/results/WFC3UVIS.im.1923282/ F814W = 2,210 s - https://etc.stsci.edu/etc/results/WFC3UVIS.im.1923285/ F606W = 571 s - https://etc.stsci.edu/etc/results/WFC3UVIS.im.1923288/ F438W = 2,083 s - https://etc.stsci.edu/etc/results/WFC3UVIS.im.1923294/ Compared to previous imaging in 12185, the indidual exposure times are increased by: F336W 585s - 1.32 times longer than GO-12185, AGN is fainter here, star cluster near SN is brighter at 3,366, so scaling counts is 4,443 F438W 694s - 5.07 times longer than GO-12185, AGN is fainter here, star cluster near SN is brighter at 2,933, scaling counts is 14,870 F814W 736s - 1.51 times longer than GO-12185, AGN maximum counts were 5,680, scaling up counts should be 8,580, less than the 48,000 DN Kept similar or same to previous program: F606W 270s in the middle betweem 160s and 400s, so kept the same F160W - kept the same because the AGN is already saturated in the previous exposures 1772210209000 237.58798714002432 (Tic-Visit :proposal-id 17777 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "21-Jul-2024 18:39:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 213904 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17777 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17777 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2635 :al-overhead-at-end 80 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17777 :visit-id "01" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2635 :al-overhead-at-end 80 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17777 :visit-id "01" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2635 :al-overhead-at-end 80 :internal-dur-at-end 270 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 3 0 552 The scheduling data was generated by CASM 34.0. CASM was run in Phase II mode. /private/var/folders/7m/h0dxnzp11zvfqtfwn_2ttggh0000gn/T/OPVisit12995403538574928181.xml Scheduling this repeat as soon as possible without causing disruption to the HST schedule and no later than April 15, 2026. I used SCHED 100 special observation requirement on the repeat. (Tic-Visit :proposal-id 17777 :visit-id "03" :proposal-version -1 :trans-version "20250929" :date "16-Mar-2026 10:26:46.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 89136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17777 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17777 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2487 :al-overhead-at-end 83 :internal-dur-at-end 134 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2867 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([02 After 01 by at most 14.0 days]) The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. WFC3_IR/F160W - estimated magnitude (AB) : 25.807 For SNR 8 we need: ~1,692 s - https://etc.stsci.edu/etc/results/WFC3IR.im.1923281/ In the previous F160W imaging, AGN counts of 51,310 are indeed higher than the full-well saturation level of ~34,000 DN. We choose the same NSAMP as the previous imaging, and do an 9-point dither patter using pos-targ, with each dither point having 2 exposures. To measure the time-varying SED, we ideally require observations to be performed taken as close together, at least within 2 months of each other. 1772317487000 274.16979010077375 (Tic-Visit :proposal-id 17777 :visit-id "02" :proposal-version -1 :trans-version "20240604" :date "05-Aug-2024 14:24:33.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 818000 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17777 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17777 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2581 :al-overhead-at-end 0 :internal-dur-at-end 717 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 1 0 Since we are measuring the SED, which is varying in time, we group the two visits with the first visit occuring after January 2025, and the second visit occuring <2 weeks after the first. We use a 2 x 9-point dither pattern.