0 Assigned ID: 5611 ----- Attempting Submission 1 (Tue Mar 26 20:17:40 GMT 2024) ----- 4th draft of Phase2 with WFC3 addressed (ACS issues addressed in 3rd draft) -1152265801 ----- Attempting Submission 1 (Wed Jul 31 15:00:55 GMT 2024) ----- ----- Attempting Submission 2 (Sun Sep 08 00:11:06 GMT 2024) ----- ----- Attempting Submission 3 (Mon Nov 04 22:15:10 GMT 2024) ----- ----- Attempting Submission 4 (Thu Nov 07 23:46:09 GMT 2024) ----- A massive protocluster at z=4.3 selected by the South Pole Telescope We request deep imaging of an SPT-selected protocluster, SPT2349-56 located at z=4.3, using HST and JWST in F435W through F1800W filters. SPT2349 possesses a very large ~10^13 Msun halo mass for any structure at z>4. Selected via millimeter-wavelength dust emission in the 2500 square degree South Pole Telescope (SPT) survey, it has been resolved by ALMA into more than 30 gas-rich galaxies, with a surrounding overdensity of LBGs and LAEs. Sensitive observations of carbon monoxide and ionized carbon with ALMA, allow assessment of the obscured star formation and gas masses of bright cluster members. The goal of this proposal is to obtain HST ACS imaging to uncover the overdensity of faint LBGs, and constrain the extincted UV properties of the SMGs. HST WFC3 + JWST NIRCam/MIRI will be used to measure the stellar properties and galaxy morphologies. The proposed HST+JWST observations leverage HST to minimize this initial JWST required to provide the imaging and photometric information for a complete picture of the obscured and unobscured stellar components of the ALMA galaxies, and the overdensity of LBGs, revealing the structure in the gas-rich galaxies that host rapid star formation and the less luminous galaxies which trace the filaments of an early collapsing structure. The combination of high resolution ALMA datasets with the proposed HST observations will allow a full characterization of the stars, gas, and dust in this cosmologically important protocluster of primordial starburst galaxies. From an outreach perspective, the high spatial resolution of the identifications of protocluster galaxies will complement the ALMA data in publicizing these high impact results. 3 filter ACS observations (g,r,i equivalents for LBG selection) 2 filter WFC3 observations (J and H band equivalents) for SED fitting. observational setup: standard setups to fill orbits in ACS typically NSAMP = 13 and SAMP-SEQ=SPARS50 for WFC3 the various choices of filters: 435w,606w, 814w in ACS for selecting lyman break galaxies 125w and 160w in WFC3 for SED fitting along with JWST bands at longer wave dither patterns, ACS-WFC-Dither-box and -line to fill available orbits accordingly The proposing team consists of members of the collaboration working to follow up and characterize the dusty, star-forming galaxies discovered by the South Pole Telescope. The team has a vast array of multiwavelength experience, including direct experience analyzing and deblending HST images very similar to those proposed here. We are also the half of the team of the JWST ERS program TEMPLATES focused on the highly dust- obscured targets of that program. PI Chapman Co-I's Gonzalez and Spilker have experience working with HST imaging, along with comparison between the rest-UV and rest-IR emission, and previous foreground/background source deblending using HST and Spitzer is published in Bothwell et al. (2013) and Ma et al. (2015). Co-I Hayward will provide needed theoretical insights; both have previously published works concerning the relationship between obscured and unobscured star formation ( Smith & Hayward 2018). Co-I Hayward also expects to perform the radiative transfer analysis necessary to compare our results with the FIRE-2 simulations. Co-I's Vieira and Phadke were primarily responsible for the design and implementation of the JWST ERS program, and expect to use the results from this program to inform the upcoming JWST observations. Large Scale Structure of the Universe Galaxies 6 false false false false false false false 4.74 true SUPPORTED CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER J2000 J2000 WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F435W POS-TARG DITHER 0.262 LINE 0.192 false false 68.14 4 18.39 ACS-WFC-DITHER-BOX 2 false POS-TARG DITHER 1.716 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 3 false POS-TARG DITHER 3.034 LINE false false 2 85.29 ACS-WFC-DITHER-LINE 4 false The scheduling data was generated by CASM 32.1.3. 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