Cannot find file \System\Volumes\Data\solaris\user1\williamj\HST-C30\TAC\C:\Users\hkito\Documents\projects\telescope_proposals\HST\Cycle30\late_time_cycle30_draft6.pdf0Assigned ID: 3215
----- Attempting Submission 1 (Fri Mar 25 13:09:10 GMT 2022) -----
HST Phase I Proposal 3215 successfully submitted.
Receipt: # 3215-1
----- Attempting Submission 2 (Fri Mar 25 13:18:44 GMT 2022) -----Following TTRB approval, visit 30 is a repeat of failed visit 25. The BETWEEN constraint has been chosen to both provide a good cadence between the last successful visit and the next planned visit, and to give the HST schedulers plenty of time to implement the new visit.294599797----- Attempting Submission 1 (Fri Jul 08 10:09:13 GMT 2022) -----
----- Attempting Submission 2 (Tue Aug 02 13:35:20 GMT 2022) -----
----- Attempting Submission 3 (Tue Aug 30 10:38:00 GMT 2022) -----
----- Attempting Submission 4 (Tue Aug 30 15:22:19 GMT 2022) -----
----- Attempting Submission 5 (Tue Apr 18 15:32:53 GMT 2023) -----
----- Attempting Submission 6 (Tue May 23 10:56:28 GMT 2023) -----
----- Attempting Submission 7 (Mon Aug 14 15:59:56 GMT 2023) -----Tripling the sample of late-time Type Ia supernovaeType Ia supernovae (SNe Ia) have long been used as standard candles to measure extragalactic distances and cosmological parameters. SNe Ia are portrayed as a homogeneous class, but there are actually several subtypes. Even the "normal" SNe Ia used for cosmology may not be homogeneous. Recently, the optical light curves of SNe Ia have been shown to slow down, relative to their earlier decline rate, at >800 days after explosion. Moreover, more luminous SNe Ia may slow down faster than less luminous objects. This correlation, which recalls the peak-light stretch-luminosity relation used to standardize SNe Ia, also hints at the existence of several production channels for normal SNe Ia, as no single explosion model can produce the full range of late-time light curves. But this new correlation is based on just 6 objects. We ask for 67 WFC3/UVIS orbits (with the F438W, F555W, and F814W filters) spread over Cycles 30-32 to observe 12 SNe Ia when they are 600-1200 days old. By tripling the sample of late-time SNe Ia, we will prove the existence of the new stretch-luminosity correlation at a significance of >5-sigma. The impact on SN cosmology will be twofold. First, a new stretch-luminosity correlation could further standardize SNe Ia and reduce systematic uncertainties. Second, strong evidence for the existence of multiple production channels for normal SNe Ia would force cosmologists to revisit their use of SNe Ia as a monolithic class. This experiment is time critical. Every year, on average, <5 SNe Ia can be used for this experiment. We are lucky to have 12 targets to work with this year; this chance may not come again during HST's remaining lifetime.In this program, we will observe the late-time decline of 12 Type Ia supernovae at late times (600 < t < 1200 days after explosion). Each target will be visited at least 5 times. Some targets will be visited a 6th time, long after they have faded below the detection limit of our observations, to obtain template images for subtractions. Each visit will be 1 orbit long and will always include the F555W filter. The first two visits, while the targets are brightest, will also include the F438W and F625W filters, respectively. We will continue to use these additional filters in subsequent visits so long as the targets are bright enough. We will download and reduce the data for each visit immediately after they are taken to determine whether the targets are still bright enough or whether we need to drop the additional filters and devote the next orbits wholly to F555W. The cadence of our observations (100-150) days is long enough that we will have enough time to alter our phase II proposal in time for the next set of observations for any specific target.
To ensure high-quality images for PSF-fitting photometry, we will use the WFC3-UVIS-3PT-LINE dither pattern. This means that, to fit in two filters, we will sometimes need to use a smaller field-of-view. Hence, we alternate between a full UVIS field of view (using UVIS, UVIS1 or UVIS2 to cover as much of the host galaxy as possible, depending on the target) and the UVIS2-C1K1C-SUB aperture. Once a given filter has been imaged once with the full aperture, we switch to the smaller one. F555W is an exception, as future visits will be devoted wholly to it, at which point we will switch from the smaller aperture to a full one.
The timing of our observations is important, as we want to catch our targets at specific phases. To that end, we use BETWEEN timing constraints for each visit. Where possible, we use a ~10-day window for schduleability.
This is a multi-cycle proposal, with 29 orbits in the first cycle, 29 in the second, and 9 in the last.Drs. Lluis Galbany, Or Graur, Griffin Hosseinzadeh, Andy Howell, Saurabh Jha, David Jones, Kate Maguire, Curtis McCully, Adam G. Riess, and Yi Yang 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, 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 (with preliminary analysis by Mr. Jamison Burke). 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, Andrew Fullard, Wolfgang Kerzendorf, and Ivo R. Seitenzahl are experts in the theory of the late-time behavior of SNe Ia. Ms. Maxime Deckers is currently working with Drs. Graur and Maguire on the late-time near-infrared behavior of SNe Ia. 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 Types6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000J2000EXT-STARSUPERNOVA TYPE IAJ2000EXT-STARSUPERNOVA TYPE IAJ2000J2000WFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falseThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit9005406203544021134.xml1667503555000321.6960069404086(Tic-Visit
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)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit7769094802337854603.xml16701722060009.599999999999994(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17191
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)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit9039021011847016108.xml167436125800059.3325062450144(Tic-Visit
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(Tic-Obset
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)
(Tic-Orbit
:proposal-id 17191
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(Tic-Obset
:proposal-id 17191
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)
(Tic-Orbit
:proposal-id 17191
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:low-sky "N"
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:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 17191
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:trans-version "20220630"
:date "23-May-2023 11:34:37.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 866240
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit9049603643324939744.xml1677270661000273.4468040003105(Tic-Visit
:proposal-id 17191
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(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:low-sky "N"
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)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit1409428431882713379.xml1689916494000108.64768153473051(Tic-Visit
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:data-volume 919728
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)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit10152910764593948135.xml1679509238000312.4766594789486(Tic-Visit
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:number-of-orbits 1
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:data-volume 919728
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:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:low-sky "N"
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)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit1746815357368000901.xml168829906500091.89999999999998(Tic-Visit
:proposal-id 17191
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 919728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3238
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 17191
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:trans-version "20220630"
:date "23-May-2023 11:37:14.0"
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:si-bright-earth-limb-angle 20.0
:data-volume 866240
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:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:obset-id "23"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3238
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit10236360996541725871.xml1680920992000257.6452488599657(Tic-Visit
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 919728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit17568797446478567328.xml1686506405000195.0(Tic-Visit
:proposal-id 17191
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 919728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:obset-id "29"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit11691696116528694828.xml1691326828000124.42869032141652(Tic-Visit
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 919728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:obset-id "25"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:al-overhead-at-end 79
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit16899688679955706693.xml(Tic-Visit
:proposal-id 17191
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 919728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17191
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit10753943465196847033.xml1682962972000269.0(Tic-Visit
:proposal-id 17191
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:si-bright-earth-limb-angle 20.0
:data-volume 919728
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)
(Tic-Obset
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)
(Tic-Orbit
:proposal-id 17191
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:dark-offset NIL
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:low-sky "N"
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)true10The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.C:\Users\hkito\AppData\Local\Temp\OPVisit3316382188963240398.xml1690306854000234.2371195002188(Tic-Visit
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(Tic-Obset
:proposal-id 17191
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)
(Tic-Orbit
:proposal-id 17191
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)true10