0
Assigned ID: 5175
----- Attempting Submission 1 (Mon Mar 25 14:10:48 GMT 2024) -----
0
----- Attempting Submission 1 (Mon Aug 12 20:27:00 GMT 2024) -----
HST Phase II Proposal 17811 successfully submitted.
Receipt: # 17811-1
----- Attempting Submission 2 (Tue Aug 13 18:37:35 GMT 2024) -----
HST Phase II Proposal 17811 successfully submitted.
Receipt: # 17811-2
----- Attempting Submission 3 (Fri Aug 16 17:41:31 GMT 2024) -----
HST Phase II Proposal 17811 successfully submitted.
Receipt: # 17811-3
----- Attempting Submission 4 (Tue Aug 20 18:28:03 GMT 2024) -----
----- Attempting Submission 5 (Wed Dec 11 23:25:43 GMT 2024) -----
Host Galaxy Imaging of Luminous Supernovae: The Missing Link of Stripped Envelope Core-Collapse Supernovae
Massive stars that have lost their hydrogen and helium envelopes generally end their lives as Type Ic (SNe Ic) core-collapse supernovae (CCSNe). However, a few percent of these stars can explode as Type I superluminous supernovae (SLSNe), which can have luminosities up to 100 times larger than SNe Ic. To date, the relationship between these two types of explosions and the connection between their progenitors remains unclear. Recently, an intermediate class of luminous supernovae (LSNe) has been unveiled, which bridged the gap between SNe Ic and SLSNe in terms of luminosity, spectroscopic properties, physical parameters, and rates. LSNe may prove to be the missing link we need to identify the progenitors of stripped-envelope CCSNe. Studying the host galaxy environments of SNe with HST has already proven to be the best way we have to infer their progenitor properties. Only HST has the depth, UV coverage, and resolution required to detect these galaxies, infer their star formation rates (SFRs) from their UV flux, and accurately pinpoint the location of the SN within their galaxies. Similar studies of about 100 SNe Ic and 80 SLSNe already exist, but only 12 LSNe have been imaged with HST, preventing a meaningful statistical comparison. Here we propose to obtain WFC3/UV imaging of all remaining 28 known LSNe to more than triple the existing sample into a statistically meaningful size, and compare with the existing population of SLSNe and SNe Ic to explore the properties of their progenitors across the entire population continuum of stripped-envelope CCSNe.
We aim to observe the host galaxies of 28 supernovae with WFC3/UVIS to measure their UV luminosity and the relation between the location of the supernova and the galaxy. Most galaxies are small dwarf galaxies a few arcsec in size. To maximize the signal while focusing on the rest-frame UV, we choose the most transmissive filters whose red edge is below about 300 nm: F300X for z<0.17, F336W for 0.17 < z < 0.41, and F390W for 0.41 < z < 0.79. We plan to observe 27 galaxies with 1 orbit, and 1 galaxy, the dimmest one, with two orbits. The program has no constraints on roll angle or when the galaxies should be observed. We plan all observations to be done with a simple 4-point dither pattern. Sources are placed on UVIS2-C1K1C-CTE aperture to maximize SNR, with the expections of large targets, which are placed on the center of UVIS2 to avoid falling off the detector. A 21 e- post-flash is used for most observations.
The proposers have extensive experience with both HST, luminous supernovae (LSNe), and superluminous supernovae (SLSNe). PI Gomez led a Cycle 27 & 28 HST program to track the evolution of a pair-instability SN candidate. Additionally, Gomez published the first comprehensive study of the population of LSNe in Gomez et al. 2022. PI Hiramatsu analyzed the late-time observations of a very peculiar supernova from a Cycle 25 program (published by Sollerman et al. 2019). Co-I Berger led a Cycle 20 program, and advised a Cycle 21 program, to observe the host galaxies of the earliest sample of superluminous supernovae (published by Lunnan et al. 2015). He also led 3 programs in Cycles 14 & 15 to study GRB host galaxies, and 3 ToO programs in Cycles 25, 27 & 28 to study GRB-associated kilonovae. Co-I Blanchard led 4 programs in Cycles 24-26 to study SLSNe and a tidal disruption event. The proposers have extensive publications records in the field of SLSNe, and LSNe, putting them in a unique position to correlate the host galaxy and SN properties.
Stellar Physics and Stellar Types
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