0
Assigned ID: 7723
----- Attempting Submission 1 (Thu Apr 16 22:19:23 GMT 2026) -----
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
Some positions were adjusted compared to phase I in order to maximize overlap with previous HST observations. While these were generally minor, for a few (~5) fields we either chose to add/subtract a second pointing due to coverage in the archive.
531565335
----- Attempting Submission 1 (Wed Aug 19 02:04:05 GMT 2026) -----
target confirmation made my APT freeze. I will try again. As noted in the comments for a few fields we added/subtracted a second pointing compared to Phase I in order to maximize overlap with previous HST observations.
Catch Them While They're Hot (And Then Not): An HST Search for Hot Failed Supernovae
Through their lives and deaths, massive stars shape nearly every area of astrophysics: chemical enrichment, ionizing radiation, compact-object formation, and gravitational-wave sources. Recent binary population models coupled with neutrino-driven explosion calculations suggest that a large fraction of massive stars at solar metallicity---of order 20--40%---may end as direct collapse to a black hole without a successful supernova (a "failed supernova"), rather than as a normal core-collapse explosion. Observational campaigns to date have produced only a handful of candidate failed SNe and have largely relied on red/optical imaging, including the largest HST search to date in F814W. Yet the same class of models predicts that well over half of failed supernovae at solar metallicity should be hot, hydrogen-poor Wolf--Rayet progenitors, with spectral energy distributions peaked in the ultraviolet. Such progenitors are faint in the filters used by past surveys, so a large fraction of failed supernovae may have evaded detection. We propose WFC3/UVIS F336W monitoring of a sample of nearby galaxies that already have deep, multi-epoch ultraviolet imaging from HST, enabling a search for luminous blue stars that disappear between epochs. The combination of HST's angular resolution in crowded environments and its UV sensitivity is critical for this test and will yield new constraints on failed-supernova rates and their implications for black-hole formation and stellar feedback.
This program will obtain new WFC3 F336W images for 40 fields overlapping nearby galaxies in order to search for failed supernova (i.e. the collapse of a massive star without a luminous explosion). We specifically chose a blue filter in order to increase our sensitivity to hot massive stars (e.g. Wolf-Rayet stars) that could have been missed by previous suveys.
Our fields were chosen such that they have (i) at least two epochs of prior HST F336W imaging and (ii) prior imaging in at least 3 filters spanning NUV to red-optical. This will allow for more detailed characterization of any candidate luminous massive star that is absent in our new observations. We do not specify orientations in order to facilitate scheduling in reduced gyro mode. We use the standard 4-point WFC3-UVIS-DITHER BOX pattern.
PI Drout is an expert in the observational study of stellar explosions and variable massive stars, including core-collapse supernovae and rare endpoints of massive-star evolution. She leads time-domain survey strategy, multi-epoch imaging analysis, and the physical interpretation of candidates in crowded galaxies.
Co-I Bowes is an expert in resolved stellar populations and HST photometry of nearby galaxies, with emphasis on completeness, contamination, and variability in crowded fields relevant to identifying disappearing luminous blue stars.
Co-I Gilkis is an expert in theoretical massive-star and binary evolution to core collapse, neutrino-driven explosion outcomes, and predicted demographics of failed supernovae including hot Wolf-Rayet progenitors and UV-focused selection effects.
Co-I Kilpatrick is an expert in time-domain astrophysics and analysis of HST imaging for transients and variable sources, including difference-style metrics and mitigation of false positives in dense stellar fields.
Co-I Laplace is an expert in modeling massive-star structures at core collapse and connecting stellar evolution and atmosphere models to observable UV/optical properties of predicted failed-SN progenitors.
Co-I O'Grady is an expert in the evolution and observational signatures of massive stars, including Wolf-Rayet and stripped-envelope channels and in distinguishing failed-SNe from other hot, variable massive-star phenomena.
Stellar Physics and Stellar Types
Stellar Populations and the Interstellar Medium
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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true
1
0
The scheduling data was generated by CASM 34.2.
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:orbit-number 1
:pcs-time 301
:si-vis-utilization 2675
:al-overhead-at-end 125
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18440
:visit-id "36"
:proposal-version -1
:trans-version "20260618"
:date "18-Aug-2026 21:49:02.0"
: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 1154992
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18440
:visit-id "36"
:obset-id "36"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18440
:visit-id "36"
:orbit-number 1
:pcs-time 301
:si-vis-utilization 2683
:al-overhead-at-end 125
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18440
:visit-id "37"
:proposal-version -1
:trans-version "20260618"
:date "18-Aug-2026 21:49:03.0"
: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 1154992
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18440
:visit-id "37"
:obset-id "37"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18440
:visit-id "37"
:orbit-number 1
:pcs-time 301
:si-vis-utilization 2683
:al-overhead-at-end 125
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18440
:visit-id "38"
:proposal-version -1
:trans-version "20260618"
:date "18-Aug-2026 21:45:03.0"
: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 1154992
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18440
:visit-id "38"
:obset-id "38"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18440
:visit-id "38"
:orbit-number 1
:pcs-time 301
:si-vis-utilization 2791
:al-overhead-at-end 125
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3092
:pcs-gap 0
)
true
1
0