S319p.223 — Probing Early Galaxy Growth and Dusty Star-Forming Systems Across Diverse Environments in the 28 deg2Herschel/Stripe82/HETDEX Field

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Aug 10th at 6:00 PM until 6:00 PM

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Author(s): Rebecca Larson7, Shardha Jogee7, Nicholas Watson7, Marco Viero3, Tim Weinzirl6, Harold W. Yorke1, Steven Finkelstein7, Casey Papovich4, Caitlin M. Casey5, Robin Ciardullo2, Caryl Gronwall2, Stephanie LaMassa8, C. Meg Urry8

Institution(s): 1. NASA Jet Propulsion Lab (JPL), 2. Pennsylvania State University, 3. Stanford University, 4. Texas A&M University, 5. University of California, Irvine, 6. University of Nottingham, 7. University of Texas at Austin, 8. Yale University

In the next few years, we will embark on an unprecedented study of how a million galaxies grow their stars and dark matter halos over a large a huge comoving volume (0.5 Gpc^3) in the cosmic web at the critical epoch (z~1.9 - 3.5), where cosmic star formation and black hole activity peak, and proto-clusters start to collapse. This study is enabled by the powerful synergy of six photometric and spectroscopic surveys, which are providing Herschel SPIRE, Spitzer IRAC, NEWFIRM K-band, DECam ugriz, and XMM X-ray imaging data, along with optical spectroscopic data from HETDEX over a very large-area (28 sq. deg.) in the Stripe82/HETDEX field. In this poster, we illustrate the power of these combined datasets and focus on studying dusty, star-forming systems (DSFSs) identified with the Herschel Stripe 82 Survey (HerS). Using the 250, 350, and 500 micron SPIRE data over our 28 sq. deg. field, we identify a number of possible high redshift (z > 4) DSFSs which will be prime candidates for follow-up observations. We discuss their properties and possible association with galaxies and quasars detected at X-ray, IR, optical, and UV wavelengths. We present examples of SED fits to DSFSs to constrain their star formation rates, redshifts and dust properties, and discuss broader implications for galaxy growth at early cosmic times. We acknowledge support from NSF grant AST-1413652 and
the JPL/NASA SURP Program.