0 Assigned ID: 5621 ----- Attempting Submission 1 (Tue Mar 26 20:25:56 GMT 2024) ----- HST Phase I Proposal 5621 successfully submitted. Receipt: # 5621-1 ----- Attempting Submission 2 (Tue Mar 26 23:23:15 GMT 2024) ----- The conversion of gas into stars on small spatial scales, and its connection to the underlying stellar backbone is key to understanding quenching in cluster galaxies. However, the dearth of high-resolution maps of the molecular gas, star formation, and stars has made it impossible to understand these processes. Recently, a new window into spatially-resolved molecular gas and far-IR emission has been opened through ALMA observations of high-redshift clusters. These gains have been mainly due to the high source density of star forming galaxies in young clusters, which allows for large multiplexing. The ALMA observations have delivered spatial and kinematic maps of the molecular gas at exquisite resolution for the first large sample of high-redshift galaxies, while the available rest-frame UV HST and ALMA FIR data have yielded star formation maps. We will combine these novel ALMA and HST data with archival imaging in F105W, F140W, and F160W to derive stellar mass maps and investigate the spatial distribution of the dominant baryonic components in main-sequence cluster galaxies at z~1.6. The 2 clusters with archival HST imaging contain galaxies in remarkable states of transformation and will be combined with analogous scheduled data on another cluster for a total sample of 29 galaxies with high-resolution spatial maps of their star formation, stellar mass, and gas. With these data we will, for the first time: 1) measure where star formation in cluster galaxies is halted (outskirts, centers, or everywhere); 2) connect deviations from scaling relationships to the stellar backbone of the galaxy; and 3) learn what role clumps play in driving mass buildup in cluster galaxies. Our team consists of co-Is with a vast range of expertise on topics related to this proposal, bridging observational to modeling and theoretical perspectives. We all have an extensive background in galaxy evolution, cluster formation, and understanding the processes that quench star formation, using both imaging and spectroscopic techniques over multiple wavelengths. All co-Is are key members of large galaxy cluster collaborations (e.g. SpARCS, GOGREEN, GCLASS). We highlight specific areas of expertise below. Photometric data reduction and analysis: Noble is the PI of the HST/UV imaging for all three clusters and the PI for the scheduled F105W, F140W, and F160W on the one cluster that is not included in this AR proposal. The rest-frame optical imaging for the two clusters in this AR proposal (J0224 and J0330) are public archival data from the See Change program. Cold gas and dust observations with ALMA: Noble is the PI of all the CO/FIR ALMA data related to the program. Theoretical predictions from cosmological hydrodynamic simulations: Bahe works with the Hydrangea simulation suite and is a core member of the next-generation COLIBRE simulation program. Quenching and galaxy structural evolution: All co-Is have expertise in this area through many related publications with GOGREEN. Galaxies 0 false false false false false false false SUPPORTED