Illegal selection: 28.Proposal Information is flagged due to submission of a Cycle 28 mid-cycle proposal through APT 2020.5, and we used the workaround of switching to DD/GO, selecting Cycle 28, then switching back to GO.-1826571830Assigned ID: 1364
----- Attempting Submission 1 (Sat Jan 30 18:09:47 GMT 2021) -----This is a cycle 28 mid-cycle proposal. We are submitting through APT 2020.5, so we used the workaround of switching to DD/GO, selecting Cycle 28, then switching back to GO.Resubmission to include 180 degree orientation shifts for all visits, to open up schedulability of our visits in early Cycle 29, due to the passing of several plan windows while HST was in safe mode in July 2021.
Resubmission with FGS3 to get constraint windows for visit 3-443923816----- Attempting Submission 1 (Thu Apr 01 03:58:54 GMT 2021) -----
----- Attempting Submission 2 (Mon Aug 09 04:05:22 GMT 2021) -----
----- Attempting Submission 3 (Wed Aug 11 20:15:48 GMT 2021) -----
HST Phase II Proposal 16504 successfully submitted.
Receipt: # 16504-3A Spectroscopically Confirmed Massively Star-forming Protocluster at z = 3.14Dense protoclusters of bright submillimeter galaxies are the suspected progenitors of today's massive clusters, but the mechanisms that govern their triggering and transition to compact quiescent galaxies by z ~ 2 are not well understood. These processes are hinted at by millimeter spectral line profiles, but are only fully resolved at sub-arcsecond scales, which cannot be imaged efficiently with ground-based telescopes in the Northern hemisphere. We propose to constrain the morphology of the stars in the two submillimeter-brightest galaxies in a newly identified, spectroscopically confirmed protocluster at z = 3.14. This requires 5 total orbits with WFC3-IR, with 3 orbits with F110W and 2 orbits with F160W. The protocluster lies in the GOODS-North and has extensive multi-wavelength coverage, but is just outside the coverage of HST/ACS and WFC3 from the original GOODS and CANDELS surveys, such that no sufficiently high-resolution imaging of this field currently exists. The two galaxies have spectroscopic redshifts from CO line scans with NOEMA, but their CO(5-4) line profiles are different, suggesting different stages or mechanisms of triggering. The 0.15'' resolution of the proposed observations will resolve close mergers and/or compact stellar counterparts. Our ~9 square arminute coverage will also serendipitously detect the near-IR counterparts of many fainter submillimeter galaxies in this dense field. The identification of advanced mergers or compact stellar counterparts in these galaxies, which can trace ongoing triggering or quenching, respectively, will be used to prioritize targets for high-resolution millimeter interferometric follow-up.We will obtain deep images of the counterparts of the four brightest SMGs in the protocluster field with the infrared channel of WFC3 in the F110W and F160W filters, to identify the extent and morphology of their stellar populations. These include GN-CL-2 and GN-CL-3, the two spectroscopically confirmed protocluster members. These galaxies are separated by more than the size of the WFC3 IR channel FoV, so we request two pointings: a northern pointing containing GN-CL-2 alone, and a southern pointing containing GN-CL-3. Splitting the observations into two pointings is necessary to avoid a bright star (2MASS J=8.34, H=7.77) in the field, which has saturated a portion of the CFHT/WIRCam images near GN-CL-1 and GN-CL-2. Our specified pointings avoid this bright star, and our orientation ranges should prevent diffraction spikes from interfering with our imaging.
We estimated exposure times using the WFC3-IR imaging calculator in F110W and F160W. We assumed that GN-CL-2 and GN-CL-3 have half-light radii of ~2.8 kpc, or 0.36 arcsec at z = 3.14, and used existing CFHT/WIRCam J and H photometry to estimate their brightnesses.
We break our observations up into four visits, with each one observing a single pointing in a single filter. The visit containing the F110W imaging of GN-CL-3 will consist of two orbits, and each of the other three visits will consist of one orbit each. These are sufficient to reach a S/N of 5 per pixel.
We will use a modified WFC3-IR-DITHER-BOX-MIN dithering pattern (pattern E4 in WFC3 IRS 2010-09) to sub-sample the PSF and step over IR blobs. Although none of our main science targets are positioned on IR blobs or the Death Star, we include this large step to maximize image quality over the whole field, given many galaxies in the WFC3 FoV may be protocluster members.Mr. Michael J. Rosenthal is a graduate student working with Dr. Amy J. Barger, and has expertise in radio interferometric observations, including co-authorship of the publication that identified the targets for this project. Mr. Logan H. Jones is a graduate student working with Dr. Barger, and has expertise working with both WFC3 data, including a first-author publication using WFC3 data in the past year, and millimeter interferometry, having led the publication that identified the targets for this project. Dr. Amy J. Barger is an expert in submillimeter galaxies and has worked with WFC3 data in two publications in the last 3 years. Dr. Lennox L. Cowie has expertise in high redshift galaxy morphologies, leading several successful proposals with WFPC2 data, and has recently had 2 first-author publications featuring WFC3 data.Galaxies3falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDCLUSTER OF GALAXIESHIGH REDSHIFT CLUSTERCoordinates are for the center of the field, which contains several submillimeter galaxies. The brightest target galaxy GN-CL-2 is at 12:35:55.88 +62:22:39.0 (+/- 2 arcsec in both RA and Dec). J and H magnitudes are for this galaxy.GN-CL-2J2000J2000J=24.0, H=23.4 (AB).CLUSTER OF GALAXIESHIGH REDSHIFT CLUSTERCoordinates are for the center of the field, which contains several submillimeter galaxies. The brightest target galaxy GN-CL-3 is at 12:35:46.64 +62:20:13.3 (+/- 2 arcsec in both RA and Dec). J and H magnitudes are for this galaxy. Also contains GN-CL-1 at 12:35:51.37 +62:21:47.2 (z=4.422) and GN-CL-4 at 12:35:39.9 +62:21:29 (z unknown).GN-CL-3J2000J2000J=25.0, H=24.0 (AB)WFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF110WPOS-TARGDITHER0.384WFC3 ISR 2010-09 IR pattern E4LINE4.793falsefalse288.3914331.798WFC3-IR-DITHER-BOX-MIN1false/private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit9645788532547348986.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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