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Assigned ID: 6192
----- Attempting Submission 1 (Wed Apr 09 00:17:03 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-1
----- Attempting Submission 2 (Wed Apr 09 23:59:34 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-2
----- Attempting Submission 3 (Thu Apr 10 19:04:49 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-3
----- Attempting Submission 4 (Thu Apr 10 20:44:56 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-4
----- Attempting Submission 5 (Thu Apr 10 20:52:02 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-5
----- Attempting Submission 6 (Thu Apr 10 22:04:21 GMT 2025) -----
HST Phase I Proposal 6192 successfully submitted.
Receipt: # 6192-6
----- Attempting Submission 7 (Fri Apr 25 14:25:42 GMT 2025) -----
0
----- Attempting Submission 1 (Thu Aug 14 14:18:34 GMT 2025) -----
The High Redshift Lyman Continuum Survey
The epoch of reionization (EoR) is a crucial event in the cosmic history. While the James Webb Space Telescope (JWST) is advancing our knowledge of reionization sources, a key factor in modeling reionization is the escape fraction of hydrogen-ionizing Lyman continuum (LyC) radiation (fesc). f_esc cannot be measured for galaxies at redshifts z>4.
HST observations have provided insights into fesc and its calibrators in local galaxies, but the evolution of galaxy properties over time raises uncertainty about the application of these calibrations to EoR systems.
We propose the High redshift LyC survey (HzLCS), a program designed to measure fesc and its indirect estimators at z=3.1-3.5. With 53 orbits of HST WFC3/UVIS and 24hours of JWST NIRISS(F200W) Wide Field Slitless Spectroscopy and imaging we will measure fesc for ~140 galaxies at these redshifts. The survey will target 20 well-separated fields, providing HST deep F336W images covering LyC wavelengths, as well as two HST optical bands, and JWST spectroscopy for redshift and galaxies' physical property measurements. By minimizing systematic uncertainties, our strategy cuts the uncertainty in fesc to 15%, matching local-universe precision and unlocking evolutionary studies just 1 Gyr after reionization ended.
We make our data public immediately.
This program images 7 fields with existing deep NIRISS spectroscopy with the WFC3/UVIS F336W filter to obtain rest-frame UV imaging data. Full orbit integrations are obtained in order to minimize post-flash and read-noise and maximize the total depth. Therefore 3 orbit vists are required to enable fully cleaning the cosmic rays. Exposures are post-flashed by 9e- to help mitigate the CTE, and reach 20e- backgrounds per pixel.
We utilize a combination of a 4 point box and 3 point line, which is similar to the 7 point pattern in ISR WFC3-2020-7. However, since the two visits may not be executed at the same position angle, we avoid trying to obtain the improved sub-pixel phasing from the 7 point pattern from that supplemental ISR as a slight change in orientation removes the benefits. We still will well sampled sub-pixel dithers in each visit which will combine sufficiently well together.
The dither pattern per visit is set 19 and 15 times larger than the default to help minimize the blotchy pattern observed in F336W imaging (i.e., similar to that seen in Rafelski et al. 2015, AJ, 150 31, Figure 15) and to dither over the chip gap with maximal number of exposures covering the chip gap while minimizing reduced FOV from lack of overlap at the edges.
In our phase I we requested an orient relative to the original NIRISS fields, but relax them (remove) here for easier scheduling as the larger WFC3 FOV over the NIRISS FOV still assures high overlap. However, we still require that the second visit for each field is wtihin +-10 degrees of the first visit, as non-overlap regions will not have sufficient exposures to fully clean the cosmic rays from orbit long exposures. If the second visit of any field is executed at a different orient, then the dither pattern would need to be revisited.
Our program is not significantly affected by the possibility of one gyro mode. If we were to go into one gyro mode, it may affect the schedulability of the second orientation. We could accept the same orient or 180 degree rotation instead of the 90 degree rotation we are currently using. Note: if we did switch orients, we would need to add an offset for the second visit to maximize the dither pattern usefullness.
The proposing team includes investigators with demonstrated expertise in all necessary components of the program, both technical and scientific.
Scientific expertise
The team is composed of experts in the measurement of f-esc, its evolution with redshift, its link with the escape of Lya radiation, and the study and characterization of indirect indicators from low redshift galaxies. We have consistently published on this and related issues, with more than 50 papers over the past decade. The team includes the core team members of the LzLCS survey.
Technical Expertise
We have expertise in both components required for the projects, the HST WFC3 UV imaging and the JWST IR slitless spectroscopy.
Our team led the reduction effort for the UV-UDF and UV-CANDELS projects and is part of the UV-Frontier Fields.
Many team members are part of the large JWST PASSAGE Survey (PI: Malkan), obtaining NIRISS slitless spectroscopy over 10s of fields.
We have a strong track record of delivering reduced data and catalogs to the public, via both MAST and IRSA archives.
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)
(Tic-Orbit
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true
3
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
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(Tic-Orbit
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(Tic-Orbit
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true
4
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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true
3
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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true
2
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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true
4
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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)
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)
true
3
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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)
true
2
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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)
(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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true
4
0
The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
(Tic-Visit
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)
(Tic-Obset
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)
true
3
0