Spitzer Warm Mission SEDS Spitzer Extended Deep Survey

Spitzer Warm Mission SEDS: Spitzer Extended Deep Survey Giovanni G. Fazio Harvard Smithsonian Center for Astrophysics and the SEDS Team

SEDS: Spitzer Extended Deep Survey • PI: Giovanni Fazio – 47 Co-I’s from 23 institutions • Primary Scientific Objective – Galaxy formation in the early Universe – Obtain first complete census of the assembly of stellar mass and black holes as a function of cosmic time back to the era of reionization – Series of secondary objectives • Unbiased survey 12 hrs/pointing at 3. 6 and 4. 5 microns ([3. 6] = 26 AB, 5 σ) in five well-studied fields (0. 9 sq deg) – 10 times area of deep GOODS survey • Total Time: 2108 hrs over 1. 5 years • No proprietary time on data

SEDS Co-Investigators Harvard Smithsonian Center for Astrophysics: Lars Hernquist, Matt Ashby, Jiasheng Huang, Kai Noeske, Steve Willner, Stijn Wuyts, T. J. Cox, Yuexing Li, Kamson Lai Max-Planck-Institut für Astronomie: Hans-Walter Rix, Eric Bell, Arjen van der Wel University of Califronia, Santa Cruz: Sandy Faber, David Koo, Raja Guhathakurta, Garth Illingworth, Rychard Bouwens NASA/GSFC: Sasha Kashlinsky, Rick Arendt, John Mather, Harvey Moseley Carnegie Observatories: Haojin Yan, Ivo Labbe, Masami Ouchi University of Pittsburgh: Jeff Newman Space Telescope Science Institute: Anton Koekemoer University of Arizona: Ben Weiner, Romeel Dave, Kristian Finlator, Eiichi Egami University of Western Ontario: Pauline Barmby Imperial College, London: Kirpal Nandra

SEDS Co-Investigators University of Chicago/KICP: Brandt Robertson Swinburne University: Darren Croton Stanford University/KIPAC: Risa Wechsler University of Florida, Gainesville: Vicki Sarajedini Astrophysikalisches Institute, Potsdam: Andrea Cattaneo University of Massachusetts, Amherst: Houjun Mo Royal Observatory Edinburgh: James Dunlop Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan: Lihwai Lin National Research Council, Herzberg Institute of Astrophysics: Luc Simard Texas A&M University: Casey Papovich Tohoku University, Japan: Toru Yamada Oxford University: Dimitra Rigopoulou University of California, Riverside: Gillian Wilson

SEDS: Scientific Objectives • Galaxy Assembly in the Early Universe – Direct study of the mass assembly back to the era of reionization. • Study stellar masses and mass functions from z = 4 - 6 • Constrain high mass end of mass function at z = 7. – Measurement of spatial clustering of galaxies • Determine the evolution of galaxy properties as a function of halo masses. – Study of identified Lyα emitters at z = 5 - 7. • High z counterparts to dwarf galaxies? • Different sample compared to dropouts – Black hole evolution at z > 6. • Study of high-z AGN number counts (constrain evolutionary models) • Relationship to stellar growth – Tests of theoretical models of galaxy assembly • Numerical simulation models to tie observational effects together

SEDS: Scientific Objectives • Auxiliary Science – Galaxy Evolution from z ~ 1 - 4 • Nature of high-z galaxies • Mass assembly of galaxies • Emergence of quiescent galaxies – Mid-infrared Variability for AGN Identification • A more universal tracer of AGN – Measurement of the Cosmic Infrared Background radiation spatial fluctuations

SEDS: Technical Aspects • Sensitivity – 12 hrs/pointing at 3. 6 and 4. 5 microns – [3. 6] = 26 AB, 5 σ (0. 15 μJy) – Robustly measure M* (reach 5 x 109 Msun at z = 6) • Field Geometry and Configuration – Clustering and large scale structure at z = 6: > 20 - 30 arcmin – Correlation length: > 5 - 10 arcmin • Number of Fields – Cosmic variance: 5 fields • Field Selection – Fields with deep auxiliary data: Extended GOODS-S, Extended GOODS-N, UDS, EGS, COSMOS/Ultra. Vista

SEDS Survey Fields

Area Coverage vs Exposure Time

IMPACT OF COSMIC VARIANCE (Bright i′ -drops in four 1 deg 2 CFHTLS; Haojing Yan) D 1(2 h, -4 d)) D 2 (10 h, +2 d) (w/COSMOS) D 4(22 h, -18 d) D 3(14 h, +53 d) (overlap EGS)) 16. 5’x 10’ GOODSSize Area D 1: D 2: D 3: D 4 ~ 1. 2: 1. 7: 1. 0: 1, 8

SEDS: Technical Aspects • Expected Number of Sources – Statistically meaningful samples – Enough to derive mass functions and perform clustering studies – Finlator models: 8000, 2000, and 200 at z = 5, 6, and 7; few at z ~ 9. • Source Selection – Conventional Lyα “dropout” technique • Z = 4, 5, 6, and 7: B, V, i, and z

SED of a Lyα Galaxy at z = 6. 6 M. Ouchi et al. 2008

Expected Cumulative Number Density at z = 6 Ivo Labbe & Haojing Yan

Spitzer Extended Deep Survey (SEDS) • Opportunity to obtain unique information on galaxy formation and evolution in the early Universe • Extensive deep survey program that will leave an important legacy for years to come.