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Spitzer Warm Mission SEDS: Spitzer Extended Deep Survey

The Spitzer Extended Deep Survey (SEDS) aims to study galaxy formation in the early Universe and obtain a complete census of the assembly of stellar mass and black holes. This unbiased survey covers five well-studied fields and will provide valuable data on the evolution of galaxies and their properties.

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Spitzer Warm Mission SEDS: Spitzer Extended Deep Survey

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

  2. 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

  3. 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

  4. 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

  5. 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

  6. 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

  7. 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/UltraVista

  8. SEDS Survey Fields

  9. Area Coverage vs Exposure Time

  10. IMPACT OF COSMIC VARIANCE(Bright i′-drops in four 1 deg2 CFHTLS; Haojing Yan) D1(2h,-4d)) D2 (10h,+2d) (w/COSMOS) D4(22h,-18d) D3(14h,+53d) (overlap EGS)) 16.5’x10’ GOODS- Size Area D1:D2:D3:D4 ~ 1.2:1.7:1.0:1,8

  11. 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

  12. SED of a Lyα Galaxy at z = 6.6 M. Ouchi et al. 2008

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

  14. 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.

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