0
Assigned ID: 459
----- Attempting Submission 1 (Fri Mar 06 12:21:35 GMT 2020) -----
HST Phase I Proposal 459 successfully submitted.
Receipt: # 459-1
----- Attempting Submission 2 (Sat Mar 07 00:08:01 GMT 2020) -----
HST Phase I Proposal 459 successfully submitted.
Receipt: # 459-2
----- Attempting Submission 3 (Sat Mar 07 00:19:23 GMT 2020) -----
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
Since visits 28-30 won't be executed within this year, I have modified the orient constraint to the prefered range.
-1717014696
----- Attempting Submission 1 (Tue Jun 30 01:20:24 GMT 2020) -----
----- Attempting Submission 2 (Tue Jul 14 19:23:31 GMT 2020) -----
HST Phase II Proposal 16276 successfully submitted.
Receipt: # 16276-2
----- Attempting Submission 3 (Wed Jul 15 19:50:33 GMT 2020) -----
----- Attempting Submission 4 (Wed Jul 15 19:54:10 GMT 2020) -----
HST Phase II Proposal 16276 failed submission.
----- Attempting Submission 5 (Wed Jul 15 20:06:55 GMT 2020) -----
----- Attempting Submission 6 (Mon Feb 01 20:52:27 GMT 2021) -----
----- Attempting Submission 7 (Thu Aug 19 23:35:31 GMT 2021) -----
----- Attempting Submission 8 (Fri Aug 27 23:14:25 GMT 2021) -----
We believe that we use the "SAME POS AS <exposure>" correctly because the grism exposure and its corresponding pre-imaging have exact same effective aperture ("GRISM1024"), target and PosTarg info.
WFC3 Spectroscopy of the Most Massive Galaxy Protoclusters at Cosmic Noon
We propose to obtain WFC3/G141 grism observations in the density peak regions of three massive protocluster fields at z=2-3, selected using coherently strong Lyman-alpha absorption from the IGM in background quasar spectra. These three protoclusters were selected using the SDSS-III quasar library of >80,000 spectra over a sky coverage of 10,000 deg^2. They have over 100 spectroscopically confirmed bright Lyman-alpha/H-alpha emitters in each system and are among the most massive protoclusters yet known at high redshifts. Previous HST imaging data have revealed a tentative population of red and compact galaxies, whose general faintness precludes ground-based spectroscopic confirmation. The WFC3/G141 grism provides the only way to efficiently confirm the redshifts of these passive galaxies through spectral features typical of old stellar populations. The goals of this proposal are: 1) to confirm the protocluster membership of red galaxies, and the redshifts of faint Lyman-alpha/H-alpha emitter candidates; 2) to characterize the stellar populations of quiescent and post-starburst galaxies, and compare the relative strengths of different quenching mechanisms (mass/internal vs. environment/external); 3) to spatially resolve the chemical profiles of the protocluster member star-forming galaxies, and measure metallicity radial gradients in a large sample of ~100 galaxies in overdense environments. The proposed observation will establish the first statistically significant benchmark for the cluster-field comparisons in the aspects of galaxy mass assembly and chemical enrichment, and provide key insights on the early evolution of the progenitors of Coma-like galaxy clusters at z~0.
In this program, we obtain in total 45 orbits of WFC3/G141 spectroscopy in the cores of three most massive galaxy protoclusters at z~2.2. For each protocluster core region, we target 5 pointings, selected based on archival HST imaging data of 1-orbit F160W exposures. Since our targets are dense fields, we need multiple orients in each field to account for possible collisions of source spectra from grism slitless spectroscopy. For each pointing, we design a set of 3 individual visits of 1-orbit depth G141 grism + F125W direct imaging exposures, with an incremental orient offset of 10-15 degrees among the three visits. One of these three visits (usually the middle one) has exactly the same orient as used in the archival imaging program, to maximize the overlap between our new G141/F125W data and the archival F160W data, so that the analysis of the sources in our fields benefit from the full HST data coverage. We use the PosTarg offset to mitigate the difference between the GRISM1024 and IR-FIX apertures of WFC3, and the offset of spectral dispersion of G141.
The reason we prefer relatively small orient offset (i.e. 10-15 degrees) rather than a large angular difference (say >45 deg) is that smaller rotation offsets have better overlap in FoV area with the archival imaging, and any angles above ~10-15 degree would provide the source spectra not similarly contaminated by the same object(s). Eventually, when combining the data taken at all three orbits for source emission line maps and 2D spectra, this orient rotation between the three visits will provide the random pixel phases we need to better sample the PSF of WFC3, and to reduce the overall average contamination. For each one of the three 1-orbit visits in each field, the observing sequence is direct, grism, offset, grism, direct. The direct images taken in the beginning/ending part of the sequence are necessary for optimal extraction and spectral calibration (wavelength + flux). The grism exposures are therefore bracketed in the middle to avoid times when the atmospheric airglow background can be substantially higher.
Our team members have extensive experience on WFC3/IR grism spectroscopy (GLASS, WISP, 3D-HST), WFC3 and ACS imaging (UVUDF, UVCANDELS, MAMMOTH, etc.). The PI, Wang, is a core member of the GLASS project, responsible for data reduction, extraction of 1D/2D grism spectra and emission line maps, and running simulations. All CoIs have extensive experience in designing and executing large programs with HST instruments, and handling the resulting large sets of complex data.
We have organized ourselves into 5 working groups: 1) Data reduction/products (Wang, Shi, Cai, Alavi); 2) Compilation of redshift catalogs (Shi, Wang, Cai, Fan, Zheng); 3) Spectrophotometric analysis of passive galaxy stellar continuum (Wang, Cai, Shi, Fan, Zheng); 4) Spatially resolved abundances/SFRs in star-forming galaxies (Wang, Bian, Alavi, Colbert); 5) Ground Based follow-up (Bian, Fan, Teplitz, Colbert, Zheng). Several team members will lead follow-up observations of the fields, with their institutional access to VLT, LBT, MMT, WIYN, Palomar, CFHT and other large ground-based telescopes.
Galaxies
Large Scale Structure of the Universe
6
false
false
false
false
false
false
false
false
SUPPORTED
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
J2000
J2000
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
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No
G141
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Imaging
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No
F125W
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Spectroscopic
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No
G141
WFC3/IR
Imaging
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No
F125W
WFC3/IR
Spectroscopic
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No
G141
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Imaging
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No
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WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
Imaging
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No
F125W
WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
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No
No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
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No
G141
WFC3/IR
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No
F125W
WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
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No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F125W
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