0 Assigned ID: 341 ----- Attempting Submission 1 (Fri Apr 05 05:20:35 GMT 2019) ----- HST Phase I Proposal 341 (clump_ar_ycguo_v2a.apt) successfully submitted. Receipt: # 341-1 ----- Attempting Submission 2 (Fri Apr 05 22:38:25 GMT 2019) ----- HST Phase I Proposal 341 (clump_ar_ycguo_v2a.apt) successfully submitted. Receipt: # 341-2 ----- Attempting Submission 3 (Fri Apr 05 23:56:31 GMT 2019) ----- HST Phase I Proposal 341 (clump_ar_ycguo_v3a.apt) successfully submitted. Receipt: # 341-3 ----- Attempting Submission 4 (Fri Apr 05 23:59:12 GMT 2019) ----- Understanding the formation of the Hubble Sequence requires detailed studies of galaxy structures over cosmic time. A prominent structural feature of distant star-forming galaxies is giant star-forming clumps. The origin and evolution of these clumps and their role in galaxy formation are still under debate. An important open question is whether clumps are long lived and migrating towards the galactic center to form bulges or if they are quickly disrupted by feedback. The keys to solve this puzzle are (1) accurate measurements of clump properties and (2) direct comparisons with models and simulations, neither of which has been sufficiently accomplished. We propose to study clumps at 0.5<z<1.5 by combining the archival data of the deepest HST UV Treasury Programs: UV images from UVUDF and HDUV as well as optical and IR images from CANDELS. With a sample of ~1,500 galaxies and ~3,000 clumps -- the largest such sample with deep HST UV coverage at this redshift range, we will (1) measure stellar mass, star formation rate, dust extinction, and stellar age of individual clumps and (2) carry out direct comparisons between observed and simulated clumps. Our result will shed light on whether clumps are building blocks of galactic bulges as well as provide stringent constrains on feedback models on sub-galactic scales. Products of our program will also enable other studies of galactic structure formation. Our team has extensive experience in reducing and analyzing HST data (UV/optical/IR) and published many highly-cited papers related to HST deep extragalactic surveys, galaxy formation, star-forming clumps, and comparisons between models and observations. Dr. Yicheng Guo has expertise in reducing and analyzing WFC3 and ACS data (the primary datasets proposed in this program) as well as studying the properties of clumps. Drs. Sandra Faber, Henry Ferguson, Mauro Giavalisco, David Koo, Marc Rafelski, and Harry Teplitz are experts in HST and galaxy formation. They have carried out several successful large HST surveys. Drs. Daniel Ceverino, Avishai Dekel, Nir Mandelker, Joel Primack, and Greg Snyder are experts in simulating and modeling galaxies. They have produced some state-of-the-art numerical simulations. Dr. Daniel McIntosh, Dr. Marc Huertas-Company, Mr. Kameswara Mantha, and Dr. Greg Snyder have expertise in generating mock HST images for direct comparisons between observations and models. Dr. Swara Ravindranath is an expert of clump formation and evolution. Dr. Timothy Carleton has expertise in modeling star formation and structure of galaxies and comparing them with observations. The proposed program consists of the following major tasks: analyzing HST data (Guo, Faber, Koo, Rafelski, and Teplitz), deriving clump properties (Ferguson, Giavalisco, Guo, and Ravindranath), generating mock HST images (McIntosh, Huertas-Company, Mantha, and Snyder) and comparing observations to simulations/models (Carleton, Ceverino, Dekel, Mandelker, and Primack). Galaxies and the IGM 0 Regular false false true false false SUPPORTED