spitzer warm mission seds: spitzer extended deep survey giovanni g. fazio harvard smithsonian center...
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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.