0Assigned ID: 521
----- Attempting Submission 1 (Fri Apr 08 15:19:37 GMT 2016) -----
HST Phase I Proposal 521 (snprog.apt) successfully submitted.
Receipt: # 521-1
----- Attempting Submission 2 (Fri Apr 08 22:22:52 GMT 2016) -----
HST Phase I Proposal 521 (snprog.apt) successfully submitted.
Receipt: # 521-2
----- Attempting Submission 3 (Fri Apr 08 22:42:37 GMT 2016) -----0----- Attempting Submission 1 (Wed Jul 20 20:22:55 GMT 2016) -----
----- Attempting Submission 2 (Thu Jan 05 15:39:23 GMT 2017) -----
----- Attempting Submission 3 (Tue May 16 17:58:24 GMT 2017) -----
HST Phase II Proposal 14645 (14645_visit2.apt) successfully submitted.
Receipt: # 14645-3
----- Attempting Submission 4 (Tue May 16 19:15:51 GMT 2017) -----
----- Attempting Submission 5 (Wed May 31 15:39:45 GMT 2017) -----
----- Attempting Submission 6 (Fri Sep 29 17:32:15 GMT 2017) -----All tools were run on Visit 4.The Stellar Origins of SupernovaeSupernovae (SNe) have a profound effect on galaxies, and have been used as precise cosmological probes, resulting in the Nobel-distinguished discovery of the accelerating Universe. They are clearly very important events deserving of intense study. Yet, even with over 9100 classified SNe, we know relatively little about the stars which give rise to these powerful explosions. The main limitation has been the lack of spatial resolution in pre-SN imaging data. However, since 1999 our team has been at the vanguard of directly identifying SN progenitor stars in HST images. From this exciting line of study, the emerging trend from 13 detections for Type II-Plateau SNe is that their progenitors appear to be relatively low mass (8 to 20 Msun) red supergiants, although more cases are needed. Additionally, evidence is accumulating that the progenitors of Type II-narrow SNe may be related to luminous blue variables. However, the nature of the progenitors of Type Ib/c SNe, a subset of which are associated with the amazing gamma-ray bursts, remains ambiguous. Furthermore, we remain in the continually embarrassing situation that we still do not yet know which progenitor systems explode as Type Ia SNe, which are being used for precision cosmology. In Cycles 16, 17, 20, 21, 22, and 23 we have had great success with our approved ToO programs. As of this proposal deadline, we have already triggered on two supernovae (SN 2016adj and SN 2016bkv) with our Cycle 23 program. We therefore propose to continue this project to determine the identities of the progenitors of 4 SNe within, generally, about 20 Mpc, which we expect during Cycle 24, through ToO observations using WFC3/UVIS.We plan for four ToO triggers during Cycle 24. If we detect one or more candidate stellar objects within a 1-sigma positional uncertainty in ACS, WFPC2, or WFC3 pre-supernova archival image(s), we will request a trigger to pinpoint the location of the SN in the pre-SN images and attempt to confirm the progenitor candidate. Our plan is to image with WFC3/UVIS, to provide the highest possible spatial resolution. Our strategy, generally, is to acquire several short-exposure dithered images in V (F555W, 10-s) or I (F814W, 30-s), for the 3 core-collapse visits (which will likely best match with the available archival image data), and in U (F336W, 20-s) or B (F438W, 20-s) for a putative, nearby (<10 Mpc) SN Ia visit, since these SNe will likely be too bright in redder bands, but fade more rapidly in the blue. We will be using the UVIS2 1Kx1K subarray near amplifier C. Since the exposures are quite short, we will also be using post-flash with 12 e- for each exposure, in order to mitigate against CTE losses. The initial Phase II observations are meant to be representative of a typical trigger. Each of the four possible ToOs has an initial placeholder position of RA(J2000)=0, Dec(J2000)=0. We will likely request triggers when the SN is still fairly bright, depending on its age at discovery, but limit this, generally, to m >14 mag. We therefore may alter exposure times and bands, depending on the expected brightness of a given SN when it is scheduled and depending on the bands of the pre-SN images available for the SN site in the HST archive. This may also result in changes in the dither strategy for a given visit. The ToOs are not intended to be high-impact, and will be requested to occur after 2 to 3 weeks from discovery, so there should be no disruption of normal scheduling.Stellar PhysicsStellar Populations0falsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IIJ2000J2000EXT-STARSUPERNOVA TYPE IIJ2000J2000EXT-STARSUPERNOVA TYPE IBJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000WFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF336WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.148592102800019.657856928535892(Tic-Visit
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