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					      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
    – Series of secondary objectives
• Unbiased survey 12 hrs/pointing at 3.6 and 4.5 microns ([3.6] = 26
  AB, 5 ) 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
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
   – Study of identified Ly 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
             SEDS: Technical Aspects

• Sensitivity
   – 12 hrs/pointing at 3.6 and 4.5 microns
   –   [3.6] = 26 AB, 5  (0.15 Jy)
   – 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
SEDS Survey Fields

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Area Coverage vs Exposure Time

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                       IMPACT OF COSMIC VARIANCE
            (Bright i-drops in four 1 deg2 CFHTLS; Haojing Yan)

                        D1(2h,-4d))                            D2 (10h,+2d)


(overlap EGS))
                                      Size Area

                                           D1:D2:D3:D4 ~ 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 Ly “dropout” technique
     • Z = 4, 5, 6, and 7: B, V, i, and z
               SED of a Ly Galaxy at z = 6.6

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                                                        M. Ouchi et al. 2008
Expected Cumulative Number
      Density at z = 6

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                                            Ivo Labbe & Haojing Yan
    Spitzer Extended Deep Survey

• Opportunity to obtain unique information on
  galaxy formation and evolution in the early

• Extensive deep survey program that will
  leave an important legacy for years to come.

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