Spitzer Warm MissionSEDS: 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

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 Co-Investigators

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/UltraVista

SEDS Survey Fields

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Area Coverage vs Exposure Time

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

D3(14h,+53d)(overlap EGS))

D4(22h,-18d)

16.5’x10’GOODS-Size Area

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

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 Lyα “dropout” technique

• Z = 4, 5, 6, and 7: B, V, i, and z

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SED of a Lyα Galaxy at z = 6.6

M. Ouchi et al. 2008

Expected Cumulative Number Density at z = 6

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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.