0
Assigned ID: 295
----- Attempting Submission 1 (Thu Apr 04 23:30:09 GMT 2019) -----
HST Phase I Proposal 295 (lensed_stars.apt) successfully submitted.
Receipt: # 295-1
----- Attempting Submission 2 (Fri Apr 05 05:59:48 GMT 2019) -----
HST Phase I Proposal 295 (lensed_stars.apt) successfully submitted.
Receipt: # 295-2
----- Attempting Submission 3 (Fri Apr 05 06:03:20 GMT 2019) -----
HST Phase I Proposal 295 (lensed_stars.apt) successfully submitted.
Receipt: # 295-3
----- Attempting Submission 4 (Fri Apr 05 07:59:48 GMT 2019) -----
ORBITAL VISIBILITY OVERRUN
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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The proposal is part of a cycle 27 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
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Updated exposure times for visits 17-24 and 1-8 to fill available window more entirely.
-1821071985
----- Attempting Submission 1 (Thu Jul 25 16:20:58 GMT 2019) -----
----- Attempting Submission 2 (Tue Jan 28 22:58:46 GMT 2020) -----
----- Attempting Submission 3 (Wed Jan 29 14:32:17 GMT 2020) -----
----- Attempting Submission 4 (Thu Mar 26 23:54:08 GMT 2020) -----
HST Phase II Proposal 15936 successfully submitted.
Receipt: # 15936-4
----- Attempting Submission 5 (Tue Mar 31 17:54:02 GMT 2020) -----
HST Phase II Proposal 15936 successfully submitted.
Receipt: # 15936-5
----- Attempting Submission 6 (Fri Apr 03 03:06:23 GMT 2020) -----
HST Phase II Proposal 15936 successfully submitted.
Receipt: # 15936-6
----- Attempting Submission 7 (Mon Apr 06 02:48:22 GMT 2020) -----
----- Attempting Submission 8 (Mon Aug 24 20:10:20 GMT 2020) -----
----- Attempting Submission 9 (Tue Aug 25 21:58:26 GMT 2020) -----
----- Attempting Submission 10 (Fri Aug 28 19:37:54 GMT 2020) -----
Overruns needed to fill available time.
Flashlights: Many Extremely Magnified Individual Stars as Probes of Dark Matter and Stellar Populations to Redshift z~2
A total of four bright microlensing events (<26.5 mag AB) of individual luminous stars at redshift z=1-2 have recently been discovered in Hubble Space Telescope observations of galaxy-cluster gravitational lenses. The frequency of these events appears to be greater than expected, and a sufficiently elevated rate would directly imply the existence of compact objects consisting of even 1-2% of dark matter. Galaxy-cluster fields also highly magnify the galaxies responsible for the reionization of the universe, yet lens models require improvement to predict the magnifications of high-redshift galaxies accurately. Finally, we lack constraints on the stellar luminosity function at z=1-2.
We propose two epochs of unfiltered ACS WFC and WFC3 UVIS imaging of each of the six Hubble Frontier
Field (HFF) galaxy clusters fields with a single-visit five-sigma limiting magnitude of 31 AB. The observations
will detect of order 100 microlensing events at three-sigma and two dozen at five-sigma significance, as well as
an equal number of always-visible pairs of stellar images. If only 2% of dark matter consists of primordial black holes, then we will detect five times as many microlensing events.
The pairs of stellar images will stringently constrain lens models, probe the abundance of low-mass dark-matter halos, and evaluate the possibility that dark matter consists of ultra-light bosons. The relative rates of microlensing events across lensed galaxies will measure variations in their stellar luminosity functions.
The proposed imaging program will, finally, identify low-redshift contaminants in James Webb Space Telescope Lyman-break galaxy samples, and detect ultra-faint galaxies.
We will acquire two epochs of deep, unfiltered ACS WFC and WFC3 UVIS imaging of each of the six Hubble Frontier Field (HFF; PI: Lotz) galaxy-cluster fields. The program will acquire simultaneous unfiltered ACS WFC and WFC3 UVIS imaging of primary and parallel fields. During each sixteen-orbit visit to each HFF cluster target, we plan to alternate between ACS WFC and WFC UVIS observations of the prime field. As described in the proposal, the detectors' differing sensitivity as a function of wavelength will provide approximate information about the spectral energy distributions of lensed sources. This alternating strategy means that we will acquire a pair of parallel fields on opposite sides of the cluster during each visit. One of these will be observed using ACS WFC and the other WFC3 UVIS.
The imaging will provide unprecedented sensitivity to the microlensing fluctuations of individual, background stars arising from objects in the foreground galaxy-cluster lenses. The rate of microlensing events will have sensitivity to even a small fraction (~1-2%) of dark matter in the form of compact objects, and constrain the luminosity function of stellar populations up to redshift z~2. Moreover, the extremely deep integrations will provide a powerful new dataset for studying the faint end of the galaxy luminosity function across a significant fraction of cosmic history and the nature of ultra-diffuse galaxies, as well as enable additional significant scientific investigations.
A primary purpose of the parallel-field observations is to carry out a control experiment to measure the rate of transients corresponding to both instrumental artifacts and stellar outbursts in galaxies in the parallel fields. We can then model the measured rate of instrumental artifacts or outbursts (controlling for magnification) in the parallel fields, and subtract the estimated rate from that measured in highly magnified galaxies in the prime field.
Dr. Patrick Kelly has extensive experience with Hubble Space Telescope (HST) imaging programs, and recently found the first example of an extremely magnified star which has a redshift of z=1.49. Dr. Jose Diego has performed the first ray tracing simulations of the effect of compact objects in a foreground galaxy lens on the light curve of a highly magnified star. Dr. Liliya Williams is an expert on gravitational lensing and galaxy-cluster modeling. Dr. Alex Filippenko has extensive expertise with HST observations and the study of transients. Dr. Masamune Oguri has recently published a paper presenting an analytic treatment of microlensing of highly magnified stars. Dr. Adi Zitrin is an expert in galaxy-cluster modeling and high-redshift galaxy populations. Dr. Tommaso Treu has led many HST programs, including campagins to study galaxy clusters, and has expertise in gravitational lensing as well as lensed galaxy populations. Dr. Nick Kaiser is an expert in the theory of gravitational lensing and developed an analytic frame for galaxy-cluster microlensing that we have used in our simulations in the proposal. Dr. Claudia Scarlata is an expert in high-redshift galaxy populations. Dr. Nathan Smith has expertise in massive stellar evolution and stellar populations. Dr. Tom Broadhurst is an expert in gravitational lensing. Dr. Dan Weisz has studied resolved stellar populations in nearby galaxies using HST. Mr. Amruth Alred, Mr. Enoch Leung, Dr. Razieh Meibody and Dr. Jeremy Lim have developed simulations of gravitational lensing where galaxy-cluster dark matter consists of ultra-light bosons. Ms. Laura Salo helped to develop the microlensing simulations. Dr. Acebron has expertise in galaxy-cluster strong lensing. Dr. Ryan Foley studies transient populations and has extensive experience with HST observations.
Cosmology
Stellar Populations
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AVAILABLE
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Hst Same orient constraint links visits (41 42 43 44 45 46 47 48)
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true
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
Hst Same orient constraint links visits (01 02 03 04 05 06 07 08)
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preferred orient as close as possible to 67 or 247 to match Hubble Frontier Field observations
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
Hst Same orient constraint links visits (01 02 03 04 05 06 07 08)
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Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 1.7 days])
Hst Same orient constraint links visits (01 02 03 04 05 06 07 08)
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Timing link suitability includes constraints ([Sequence (17 18 19 20 21 22 23 24) within 1.7 days])
Hst Same orient constraint links visits (17 18 19 20 21 22 23 24)
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Timing link suitability includes constraints ([Sequence (17 18 19 20 21 22 23 24) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (17 18 19 20 21 22 23 24) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (17 18 19 20 21 22 23 24) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (17 18 19 20 21 22 23 24) within 1.7 days])
Hst Same orient constraint links visits (17 18 19 20 21 22 23 24)
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Timing link suitability includes constraints ([Sequence (09 10 11 12 13 14 15 16) within 1.7 days])
Hst Same orient constraint links visits (09 10 11 12 13 14 15 16)
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Timing link suitability includes constraints ([Sequence (09 10 11 12 13 14 15 16) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (09 10 11 12 13 14 15 16) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (09 10 11 12 13 14 15 16) within 1.7 days])
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Timing link suitability includes constraints ([Sequence (09 10 11 12 13 14 15 16) within 1.7 days])
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