May 24: Initial submission
May 24: re-submitting with a revised version
May 24: re-submitting with minor revisions
-274080109
Assigned ID: 4566
----- Attempting Submission 1 (Wed May 24 19:59:58 GMT 2023) -----
HST Phase I Proposal 4566 successfully submitted.
Receipt: # 4566-1
----- Attempting Submission 2 (Wed May 24 21:58:23 GMT 2023) -----
HST Phase I Proposal 4566 successfully submitted.
Receipt: # 4566-2
----- Attempting Submission 3 (Wed May 24 23:30:27 GMT 2023) -----
Sep 13: Initial Phase II submission
Nov 3: Added ORIENT constraints for Visits 02 and 03 (after PCR approval from TTRB)
2040841066
----- Attempting Submission 1 (Wed Sep 13 22:47:27 GMT 2023) -----
----- Attempting Submission 2 (Fri Nov 03 22:17:21 GMT 2023) -----
Unlocking the rich potential of JWST slitless spectroscopy with the help of HST: an optical follow-up campaign
The first round of JWST data are already revolutionizing the field of galaxy evolution. The large amount of slitless spectroscopic data collected in Cy1 are well poised to extend our knowledge about galaxies at the cosmic high-noon (z=1 to 3) down to unprecedented stellar masses of ~10^8 Msol. The pure-parallel PASSAGE program is currently the largest-area survey with contiguous, deep 1-2.2 micron JWST grism data. Unfortunately, the corresponding photometric coverage is severely limited making it extremely challenging to accurately recover fundamental physical properties of galaxies such as their stellar masses and dust attenuation, which are vital for answering the majority of galaxy evolution science questions.
Here, we propose to follow-up 7 premier PASSAGE fields with 3-band grism coverage (1-2.2 micron) from JWST to obtain the crucial rest-frame UV imaging needed to accurately measure their physical properties. We request a combination of WFC3/UVIS F475W, F625W and ACS/WFC F814W imaging (1 orbit each) for a total of 21 orbits (3 per field). These data in combination with PASSAGE will enable: (i) accurate stellar mass estimates for hundreds of galaxies over 0.5<z<3.5 and constrain the low-mass end of the star-forming main sequence and mass-metallicity relation; (ii) spatially resolved comparison between UV and Halpha to reveal a resolved picture of star-formation burstiness in galaxies and their mass assembly; and (iii) accurate measurement of the stellar dust attenuation and the relative strengths of stellar vs. nebular dust components in star-forming galaxies at z~2.
This program is designed to acquire follow-up HST optical imaging for seven fields from the JWST-PASSAGE survey, which is a pure-parallel JWST/NIRISS slitless-spectroscopy program obtaining grism data in up to 3 filters (F115W, F150W, F200W). This HST follow-up program specifically prioritizes the best PASSAGE fields that have grism data in all 3 filters to acquire complementary and crucial optical imaging.
This follow-up program aims to obtain high-resolution imaging with WFC3/UVIS in F475W, F625W filters and with ACS/WFC in F814W. With 1 orbit of imaging in each filter, these observations will reach an imaging depth of 27.3, 27.0, 27.1 AB in F475W, F625W, F814W respectively, which is comparable to the depths of PASSAGE data for the selected fields. We opt to use WFC3/UVIS for F475W and F625W for its better imaging quality and fewer hot pixels while maintaining similar throughput as ACS/WFC, whereas ACS/WFC outperforms with higher throughput for the F814W filter. The total integration time for our observations is split into 3 dithered frames for each filter. Given our exposure times, we do not need to apply post-flash. The total orbit allocation adds to 21 orbits -- 1 orbit per each of the 3 imaging filters for a total of 7 target fields.
The field-of-view for both WFC3/UVIS and ACS/WFC is large enough compared to JWST/NIRISS such that we do not require telescope orient constraints for our observations. We specifically target the field centers of the JWST observations and use the UVIS-CENTER and WFCENTER apertures for WFC3/UVIS and ACS/WFC observations, respectively, to ensure maximal overlap between the HST filters as well as with the existing JWST data.
The members of the proposing team have extensive scientific and technical experience with using HST imaging to study galaxy evolution. Our team includes members who are part of the PASSAGE collaboration and are well-versed with the JWST slitless spectroscopy data.
Scientific expertise:
Our team includes experts on interpreting galaxy physical properties from observational data in the context of advancing our knowledge on galaxy evolution. Drs. Alavi, Atek, Hayes, Malkan, Nedkova, Mehta, Scarlata, Rafelski, Teplitz, Treu have led several studies focused on studying the physical properties of galaxies at redshifts of 1-3 using WFC3 and ACS data. Drs. Alavi, Battisti, Colbert have led several works investigating stellar and nebular dust attenuation measurements of high-z galaxies. Drs. Mehta, Wang, Vulcani are experts on spatially resolved mapping of z~1 to 3 galaxies to study the star-formation gradients, star-formation histories, dust properties and gas metallicity. Drs. Atek, Baronchelli, Battisti, Mehta, Wang have led multiple studies using slitless spectroscopy data to measure redshifts, emission line features as well as analyze galaxy masses, sizes, star-formation properties, metallicity and ionization states.
Technical expertise:
Many of the team members have led or been an integral are part of the JWST surveys PASSAGE (PI: Malkan), GLASS-ERS (PI: Treu) as well as HST surveys WISP (PI: Malkan), UV-UDF (PI: Teplitz), UV-CANDELS (PI: Teplitz), UV-Frontier Fields (PI: Scarlata), GLASS (PI: Treu), LaCOS (PI: Hayes), MAMMOTH (PI: Wang). Drs. Alavi, Mehta, Rafelski, Wang have extensive hands-on experience with HST observing, reducing HST imaging data and performing precise photometry. Our team members are a core part of several slitless surveys (HST-based WISP, GLASS and now JWST-based GLASS, PASSAGE) and are experts on slitless spectroscopy. Drs. Mehta, Nedkova, Rafelski are experts on using SED fitting to estimate photometric redshifts and galaxy physical properties.
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:dark-utilization 0
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:low-sky "N"
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)
(Tic-Orbit
:proposal-id 17461
:visit-id "06"
:orbit-number 2
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:si-vis-utilization 2622
:al-overhead-at-end 116
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
false
2
0
HOPR repeat of second orbit of visit 06.
(Tic-Visit
:proposal-id 17461
:visit-id "06"
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:trans-version "20240604"
:date "01-Jul-2024 16:40:35.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
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:si-bright-earth-limb-angle 20.0
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17461
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)
(Tic-Orbit
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:dark-offset NIL
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)
(Tic-Orbit
:proposal-id 17461
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:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
false
2
0
(Tic-Visit
:proposal-id 17461
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:date "01-Jul-2024 16:41:13.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "27"
:si-bright-earth-limb-angle 20.0
:data-volume 852672
:tdrss-contact-duration 0
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)
(Tic-Obset
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(Tic-Orbit
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:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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false
1
0
The scheduling data was generated by CASM 31.1.
CASM was run in Phase II mode.
1713761785000
233.84863183918958
(Tic-Visit
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:trans-version "20230626"
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(Tic-Obset
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)
(Tic-Orbit
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:orbit-number 2
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:dark-offset NIL
:dark-utilization 0
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)
false
2
0
1713676911000
234.80498372311985
(Tic-Visit
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:number-of-orbits 1
:saa-model "27"
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:tdrss-contact-duration 0
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)
(Tic-Obset
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(Tic-Orbit
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:dark-offset NIL
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false
1
0