0Assigned ID: 6593
----- Attempting Submission 1 (Thu Apr 10 18:28:22 GMT 2025) -----The number of orbits used exceeds the number allocatedupdated Visit 14 with all NUV observations and visit 15 with FUV+NUV as two different options depending on scheduling-1538170813----- Attempting Submission 1 (Wed Aug 27 21:07:47 GMT 2025) -----
----- Attempting Submission 2 (Wed Jan 21 17:08:45 GMT 2026) -----
----- Attempting Submission 3 (Thu Jan 22 14:34:59 GMT 2026) -----
HST Phase II Proposal 18073 successfully submitted.
Receipt: # 18073-3
----- Attempting Submission 4 (Thu Jan 22 15:41:12 GMT 2026) -----
----- Attempting Submission 5 (Thu Feb 12 05:28:16 GMT 2026) -----
HST Phase II Proposal 18073 successfully submitted.
Receipt: # 18073-5
----- Attempting Submission 6 (Thu Feb 12 05:36:26 GMT 2026) -----All errors are irrelevant (object has already been observed)Using Early FUV Spectra of Type IIP/L Supernovae to Elucidate Mass Loss in Red SupergiantsRed supergiants, the progenitors of Type IIP/L supernovae lose a significant fraction of their initial mass during their lifetimes. However, there is no first-principle description of this mass loss and empirical prescriptions vary by orders of magnitude. On top of this uncertainty, recent optical supernova observations show periods of enhanced mass-loss occur just prior to explosion which are not described by any model. It is not known what fraction of red supergiants experience this kind of eruptive mass loss. While optical light curves and spectroscopy can probe the most extreme mass-loss rates, the UV is significantly more sensitive to interaction between the supernova ejecta and circumstellar material, probing mass-loss rates from nominal red supergiant winds to the strongest outbursts. Additionally, during the first week of evolution, while the optical is relatively featureless, the FUV is full of high-ioniztion and strong resonance lines which provide information about the metalicity of the progenitor star, temperature and density of the supernova ejecta, and the composition of the circumstellar material. These observations are also critical for interpreting the growing number of supernovae discovered at high redshift. However, early FUV observations are challenging: only ~1 infant supernova per year is observable with HST. In this proposal, we request a disruptive ToO observation to study a nearby, infant, Type IIP/L supernova in the FUV and NUV. These observations will map the final phases of red supergiant mass loss, connect them to the properties of the supernova and progenitor star, and shed light on the UV diversity of supernovae.We will trigger this ToO on a Type II supernova that is UV bright and discovered within 24 hours of explosion. We would like the First visit to execute as soon as possible with the second visit executing a day later and the third visit a day after that. The final visit will execute 7 days after the last visit.
We request a full GS acquisition at the beginning of each orbit of the first three visits as the supernova will change on the timescale of a day and thus these observations are not repeatable.
We use a fixed target as a placeholder for the real target to easily vet the visibility of new candidates. The coordinates will be updated before the ToO trigger is submitted.The Distance less than 40 Mpc team has extensive experience with UV observations and analyzing CSM interaction in hydrogen-rich supernovae at early and late times. We are members of the Global Supernova Project which has access to robotic telescopes for imaging and spectroscopy around the world and routinely PI programs for late time spectra on Keck, MMT, and the Large Binocular Telescope.
K. A. Bostroem is a former member of the STIS team at STScI and has extensive experience with the STIS, Swift, Gemini, and Keck data reduction. Her research focuses on understanding the progenitors of hydrogen-rich CC SNe. She is the PI of programs to obtain HST/STIS UV data SN2022acko and SN2023ixf and already published a paper on Early CSM interaction in the optical spectra of SN 2023ixf.
S. Valenti is the PI of a Cycle 31 program and a DD program to obtain HST/STIS FUV and NUV spectra of SN 2023ixf. He is the co-PI of DLT40. He has worked comprehensively on core collapse supernovae (CC SNe).
M. Lundquist is an active member of the DLT40 team and specializes in the reduction and analysis of Gemini and Keck observations. He is currently a staff astronomer at the W. M. Keck Observatory. Prior to joining the DLT40 team, he worked as a Gemini Science Fellow at the Gemini Observatories.
J. Andrews is an active member of the DLT40 team, has expertise observing with HST/STIS, and is an assistant astronomer at the Gemini Observatory. Her research focuses on characterizing the progenitors of core collapse (CC) SNe, specifically focusing on their mass-loss history via circumstellar interaction.
D. Sand is the co-PI of the DLT40 survey and an expert in the progenitors of Type Ia SNe and SN environments. He has extensive experience with Swift, and Gemini observations of SNe and their environments.
M. Shrestha is a Postdoctoral Research Associate at the University of Arizona. Her research focuses on the transients such as long gamma-ray bursts, core collapse (CC) SNe, and kilonova. She is part of DLT40 and SAGUARO collaborations.
J. Jencson is an active member of the DLT40 team and has extensive experience in reducing and analyzing Swift observations of transients. His research focuses on multi-wavelength studies of hydrogen-rich transients and searches for dust-obscured transients and faint/failed SNe.
G. Hosseinzadeh is an expert in early SN~Ia light curves and has experience analyzing early UV data.
J. Pearson is focusing her thesis research on understanding the progenitors and environments of CC SNe and is an active member of the DLT40 team.
Y. Dong is an senior graduate student in the DLT40 team and has experience analyzing both CC~SNe and SN~I.
N. Meza is a graduate student in the DLT40 team focusing his thesis work on CC~SNe.
E. Hoang is a graduate student in the DLT40 team focusing on stripped-envelope SNe.
D. Janzen is a member of the SkyNet team which is responsible for maintaining the telescopes that the DLT40 team uses for their search.
S. Jha is an expert in Type Ia supernovae and the PI of a program on SALT to obtain spectra of supernova transients. SALT is ideally located for obtaining rapid classification spectra of supernovae discovered by our Australian telescope.
A. P. Ravi is a postdoc in the DLT40 team and has expertise in high energy emission from supernovae. He leads the UC Davis NIR observing program.
D. Mehta is a graduate student in the DLT40 team focusing on short plateau SNe.
L. Kwok is the PI of a Cycle 3 JWST proposal to observe SNe~Ia from infancy until nebular phase. She is an expert in the mid-infrared properties of both normal and peculiar SNe~Ia.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IINOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300Timing link suitability includes constraints ([02 After 01 by 0.7 to 1.2 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
First epoch should be executed as soon as possible after trigger
For SN with initial brightness around r=17 mag(Tic-Visit
:proposal-id 18073
:visit-id "01"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:26.0"
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:data-volume 404448
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:coron NIL
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(Tic-Obset
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(Tic-Obset
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(Tic-Obset
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(Tic-Orbit
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:visit-id "01"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2489
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:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18073
:visit-id "01"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2356
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:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)
(Tic-Orbit
:proposal-id 18073
:visit-id "01"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2362
:al-overhead-at-end 0
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
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)true30Waiting for a suitable supernova to explode.
I understand this response time is likely a lower limit on what STScI is capable of but the sooner the better for this programTiming link suitability includes constraints ([06 After 05 by at most 0.3 days] [07 After 05 by at most 0.3 days] [08 After 05 by 0.7 to 1.2 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
First epoch should be executed as soon as possible after trigger
For SN with initial brightness around r=17 mag1769448903000344.3352446732963(Tic-Visit
:proposal-id 18073
:visit-id "05"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:26.0"
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:number-of-orbits 1
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:data-volume 87408
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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(Tic-Orbit
:proposal-id 18073
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:si-vis-utilization 2489
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true10Timing link suitability includes constraints ([06 After 05 by at most 0.3 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
First epoch should be executed as soon as possible after trigger
For SN with initial brightness around r=17 mag1769454533000344.40923021757703(Tic-Visit
:proposal-id 18073
:visit-id "06"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:26.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:data-volume 174416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18073
:visit-id "06"
:obset-id "06"
:pcs-mode "FGS"
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(Tic-Orbit
:proposal-id 18073
:visit-id "06"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2356
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true10Timing link suitability includes constraints ([07 After 05 by at most 0.3 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
First epoch should be executed as soon as possible after trigger
For SN with initial brightness around r=17 mag1769460390000345.72147255407947(Tic-Visit
:proposal-id 18073
:visit-id "07"
:proposal-version -1
:trans-version "20250929"
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:data-volume 142624
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18073
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18073
:visit-id "07"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2362
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true10Timing link suitability includes constraints ([02 After 01 by 0.7 to 1.2 days] [03 After 02 by 0.7 to 1.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Second epoch should be executed 24 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 1(Tic-Visit
:proposal-id 18073
:visit-id "02"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 404448
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:visit-id "02"
:obset-id "02"
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(Tic-Obset
:proposal-id 18073
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:obset-id "A2"
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(Tic-Obset
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:visit-id "02"
:obset-id "B2"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18073
:visit-id "02"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2489
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18073
:visit-id "02"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2356
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18073
:visit-id "02"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2362
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
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:low-sky "N"
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)true30Waiting for a suitable supernova to explode.Timing link suitability includes constraints ([08 After 05 by 0.7 to 1.2 days] [09 After 08 by at most 0.3 days] [10 After 08 by at most 0.3 days] [11 After 08 by 0.7 to 1.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Second epoch should be executed 24 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11769527755000345.37674246717097(Tic-Visit
:proposal-id 18073
:visit-id "08"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 87408
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:visit-id "08"
:obset-id "08"
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)
(Tic-Orbit
:proposal-id 18073
:visit-id "08"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2489
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true10Timing link suitability includes constraints ([09 After 08 by at most 0.3 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Second epoch should be executed 24 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11769533401000345.4515956828167(Tic-Visit
:proposal-id 18073
:visit-id "09"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:coron NIL
)
(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([10 After 08 by at most 0.3 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Second epoch should be executed 24 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11769539293000345.72147255407947(Tic-Visit
:proposal-id 18073
:visit-id "10"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:29.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:data-volume 142624
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
:proposal-id 18073
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:dark-offset NIL
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)true10Timing link suitability includes constraints ([03 After 02 by 0.7 to 1.0 days] [04 After 03 by 6.0 to 8.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Third epoch should be executed 24 hours after second visit and 48 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 1(Tic-Visit
:proposal-id 18073
:visit-id "03"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:29.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 2
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:data-volume 230048
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:coron NIL
)
(Tic-Obset
:proposal-id 18073
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
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(Tic-Obset
:proposal-id 18073
:visit-id "03"
:obset-id "A3"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18073
:visit-id "03"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2477
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
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)
(Tic-Orbit
:proposal-id 18073
:visit-id "03"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2363
:al-overhead-at-end 0
:internal-dur-at-end 360
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true20Waiting for a suitable supernova to explode.Timing link suitability includes constraints ([11 After 08 by 0.7 to 1.0 days] [12 After 11 by at most 0.3 days] [13 After 11 by 6.0 to 8.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Third epoch should be executed 24 hours after second visit and 48 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11769612447000346.506102574991(Tic-Visit
:proposal-id 18073
:visit-id "11"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:30.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 87408
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18073
:visit-id "11"
:obset-id "11"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18073
:visit-id "11"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2477
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2987
:pcs-gap 0
)true10Timing link suitability includes constraints ([12 After 11 by at most 0.3 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
Third epoch should be executed 24 hours after second visit and 48 hours after first visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11769623739000346.6577401728691(Tic-Visit
:proposal-id 18073
:visit-id "12"
:proposal-version -1
:trans-version "20250929"
:date "22-Jan-2026 08:39:30.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 142640
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18073
:visit-id "12"
:obset-id "12"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18073
:visit-id "12"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2363
:al-overhead-at-end 0
:internal-dur-at-end 360
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)true10Timing link suitability includes constraints ([04 After 03 by 6.0 to 8.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
fourth epoch should be executed 7 days after third visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 1(Tic-Visit
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)true40Waiting for a suitable supernova to explode.Timing link suitability includes constraints ([13 After 11 by 6.0 to 8.0 days])The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.Please put a full GS acq at the beginning of each orbit so if one orbit fails the others have a chance of succeeding. I can adjust the exposure times if needed
fourth epoch should be executed 7 days after third visit
For SN with initial brightness around r=17 mag
If possible execute at same orientation as visit 11770137675000353.8241883030023(Tic-Visit
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)true4043NUV only visit if this cannot be scheduled until later(Tic-Visit
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