NOAO >   Observing Info >   Approved Programs >   2013B-0438

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Proposal Information for 2013B-0438


PI: Casey Papovich, Texas A&M University, papovich@physics.tamu.edu
Address: Dept of Physics and Astronomy, 4242 TAMU, College Station, Texas 77843-4242, United States

CoI: Robin Ciardullo, Penn State
CoI: Gavin Dalton, Oxford
CoI: Darren DePoy, Texas A&M
CoI: Niv Drory, UNAM
CoI: Steven Finkelstein, Univ. of Texas-Austin
CoI: Eric Gawiser, Rutgers
CoI: Karl Gebhardt, UT Austin
CoI: Caryl Gronwall, Penn State
CoI: Shardha Jogee, UT Austin
CoI: Jennifer Marshall, Texas A&M
CoI: Nicola Mehrtens, Texas A&M
CoI: Erin Mentuch, UT Austin
CoI: Vithal Tilvi, Texas A&M
CoI: Sarah Tuttle, UT Austin
CoI: Risa Wechsler, Stanford
CoI: Peter Behroozi, Stanford
CoI: Rachel Somerville, Rutgers
CoI: Greg Zeimann, Penn State
CoI: Houri Ziaeepour, MPE-Garching

Title: DECam u-Band Imaging of the HETDEX/SHELA field

Abstract: We propose deep DECam u-band and additional riz-band imaging of a 23 deg^2 legacy field in SDSS Stripe 82, centered on 1h24m, +0d. This region will have complete spectroscopic coverage from HETDEX, including redshifts for ~300,000 galaxies between 1.9<$z$<3.5, deep 3.6 and 4.5 micron imaging from Spitzer/IRAC for about 400,000 galaxies over this redshift range, and deep far-IR data from Herschel/SPIRE. The Dark Energy Survey (DES) will provide griz imaging of this field, but DES provides \textitno u-band imaging. Our proposed u-band observations are highly important to build a complete census of galaxies at 1.9<$z$<3.5 because the u-g color cleanly distinguishes between galaxies 2<$z$<3.5 and star- forming galaxies at low-z, which are otherwise degenerate redshift solutions. Our science goal is to measure simultaneously the stellar mass-dark-matter halo mass \textitfunction for galaxies in the critical epoch 1.9<$z$<3.5. The large area of our survey covers a co-moving volume of ~0.5 Gpc^3, large enough to contain several hundred Virgo- and group-sized progenitors. Therefore, our survey will measure the growth of stellar mass as a function of halo mass \textitand environment with statistically meaningful samples to separate the effects of physical processes associated with mass from those associated with environment.


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