0 Assigned ID: 1338 ----- Attempting Submission 1 (Fri Jan 29 14:26:19 GMT 2021) ----- HST Phase I Proposal 1338 successfully submitted. Receipt: # 1338-1 ----- Attempting Submission 2 (Fri Jan 29 21:01:46 GMT 2021) ----- HST Phase I Proposal 1338 failed submission. ----- Attempting Submission 3 (Fri Jan 29 21:05:30 GMT 2021) ----- Rescheduleing visit 02 so that it falls before August 15 (the edge of the last observability window). 1347803435 ----- Attempting Submission 1 (Mon Mar 22 15:27:58 GMT 2021) ----- ----- Attempting Submission 2 (Mon Mar 22 19:34:14 GMT 2021) ----- ----- Attempting Submission 3 (Wed Mar 31 20:08:50 GMT 2021) ----- ----- Attempting Submission 4 (Thu Apr 08 12:20:54 GMT 2021) ----- HST Phase II Proposal 16497 successfully submitted. Receipt: # 16497-4 ----- Attempting Submission 5 (Thu Apr 08 12:27:50 GMT 2021) ----- HST Phase II Proposal 16497 successfully submitted. Receipt: # 16497-5 ----- Attempting Submission 6 (Fri Apr 09 15:08:50 GMT 2021) ----- ----- Attempting Submission 7 (Fri Jun 25 08:43:12 GMT 2021) ----- ----- Attempting Submission 8 (Thu Jul 22 18:46:39 GMT 2021) ----- ----- Attempting Submission 9 (Mon Jul 26 18:36:33 GMT 2021) ----- The Near-Infrared Plateau of Type Ia Supernovae We ask for 8 WFC3 orbits to observe four Type Ia supernovae (SNe Ia) when they are ~230-430 days past maximum light. At these phases, normal SNe Ia have been shown to undergo a plateau phase in the near-infrared (NIR) while continuing to decline in the optical. Our sample consists of two normal SNe Ia and two peculiar SNe Iax. With two visits per SN during this phase range, we will use observations in F125W (J), F160W (H), F336W (U), and F350LP (optical) to: (1) confirm the J-band plateau for normal SNe Ia; (2) test whether the plateau is caused by scattering of photons from the UV/optical to the NIR; (3) test whether SNe Iax also exhibit a NIR plateau; and (4) detect the surviving white dwarf progenitors of SNe Iax. At late times, observations drive theory, and ours will help shed light on the progenitor and explosion physics of both normal SNe Ia and their peculiar Iax cousins. We will use WFC3 to observe four Type Ia supernovae with two visits to each supernova. Every visit will be composed of a single orbit. SNe 2020hvf and 2020uxz are brighter than 2020udy and 2020kyg. The brighter supernovae will be observed with four filters: WFC3/UVIS F350LP and F336W and WFC3/IR F125W and F160W. For the fainter supernovae, we will drop the F336W filter. The IR observations use a 3pt dither. In orbits that include both F336W and F350LP, we will use a 2pt dither (to limit overheads). In orbits where we only use F350LP, we will use a 3pt dither instead. Each visit has been given a time window of ~11 days to increase the scheduleability of the observations. The same is true for the total exposure time per orbit.; for two of our targets (2020uxz and 2020udy), we do not make full use of the orbits in order to maximize their scheduleability. The observations from the first visit to each supernova will be reduced and analyzed immediately in order to try and localize the supernova and measure its brightness in all filters. This will inform any potential changes to the filter loadout and exposure times for the second visit (e.g., if the supernova does not appear in a certain filter or is expected to drop out in that filter, we may choose to shift the exposure time into another filter in which the supernova will definitely be visible). We chose WFC3 UVIS1-2k2k subrasters for the FOV, but only because the UVIS1 full FOV (which we usually use) seemed to cost too much in overhead. For each target, the specific subraster (e.g., 2k2a or 2k2d) was chosen to capture as much of the host galaxy as possible in the FOV, while still including the target itself. Drs. Kate Maguire, Curtis McCully, Lluis Galbany, Or Graur, Griffin Hosseinzadeh, Andy Howell, Saurabh Jha, and Adam G. Riess are all expert supernova (SN) observers. Dr. Graur has used HST+WFC3 to lead several experiments similar to the one proposed here, with SN 2012cg (Graur et al. 2016), SN 2015F (Graur et al. 2018a), ASASSN-14lp (Graur et al. 2018b), SN 2014J (Graur 2019), and several SNe Ia in the near-infrared (Graur et al. 2020). Dr. Riess has a long record of observing SNe with HST. Drs. McCully and Jha are experts in the study of SNe Iax. Drs. McCully, Hosseinzadeh, and Howell form the core of the Las Cumbres Observatory's Global Supernova Project, which has provided early-time observations of the SNe in this proposal. Dr. Michael M. Shara is an expert in HST observations of various types of transients. Dr. David R. Zurek is an expert in the processing of HST images. Drs. Robert Fisher, Ken Shen, and Ivo R. Seitenzahl are experts in SN explosion models and nucleosynthesis. Finally, Dr. Armin Rest is a world leader in the detection and analysis of light echoes. Dr. Or Graur will serve as PI of this program, and Dr. Saurabh Jha will serve as its US administrative Co-I. Stellar Physics and Stellar Types 3 false false false false false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE IA J2000 EXT-STAR SUPERNOVA TYPE IA J2000 J2000 EXT-STAR SUPERNOVA TYPE IA J2000 J2000 EXT-STAR SUPERNOVA TYPE IA J2000 J2000 WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F336W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F336W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/UVIS Imaging No No F350LP WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/UVIS Imaging No No F350LP POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1 false POS-TARG DITHER 0.636 LINE false false 2 41.788 WFC3-IR-DITHER-LINE 2 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 3 false The scheduling data was generated by CASM 29.2. 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