The Spitzer Extended Deep Survey (SEDS) Spitzer Warm Mission Kai Noeske, Giovanni G. Fazio Harvard-Smithsonian Center for Astrophysics and the SEDS Team The Origin of Galaxies: Lessons from the Distant Universe Obergurgl, Austria, 16 Dec 2009 SEDS: The Spitzer Extended Deep Survey - Overview - PI: Giovanni Fazio, CfA 47 Co-Is from 23 institutions Primary Scientific Objective Galaxy formation in the early Universe 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 at 3.6 and 4.5 microns 12 hours/pointing ([3.6] = 26 AB, 5 ) 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 Harvard-Smithsonian CfA: Lars Hernquist, Matt Ashby, Jiasheng Huang, Kai Noeske, Steve Willner, Stijn Wuyts, T.J. Cox, Yuexing Li, Kamson Lai Max-Planck-Institut fr 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: Brant Robertson Swinburne University: Darren Croton Stanford University/KIPAC: Risa Wechsler University of Florida, Gainesville: Vicki Sarajedini Astrophysikalisches Institut, Potsdam: Andrea Cattaneo University of Massachusetts, Amherst: Hojun 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: The Spitzer Extended Deep Survey - Motivation - Only Spitzer can see redward of 4000A break at high z => stellar masses/populations, photo-zs Warm Mission only chance to deeply map large area at >3 microns => comprehensive census of: stellar mass assembly in the early universe (L* at z=6) high-z AGN star formation into era of reionization Best target finder for JWST, ALMA, ELTs, large radio arrays 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* (5 x 10 9 Msun) at z=6 Field Geometry and Configuration Clustering and large scale structure: fields > arcmin (>3-4x correlation length of massive galaxies at z=6) Number of Fields Cosmic variance: 5 fields Field Selection Fields with deep auxiliary data: Extended GOODS-S, Extended GOODS-N, UDS, EGS, COSMOS/UltraVista 3 Epochs, 6 months apart -> variability Expected Cumulative Number Density at z = 6 Ivo Labbe & Haojing Yan 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* (5 x 10 9 Msun) at z=6 Field Geometry and Configuration Clustering and large scale structure: fields > arcmin (>3-4x correlation length of massive galaxies at z=6) Number of Fields Cosmic variance: 5 fields Field Selection Fields with deep auxiliary data: Extended GOODS-S, Extended GOODS-N, UDS, EGS, COSMOS/UltraVista 3 Epochs, 6 months apart -> variability 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* (5 x 10 9 Msun) at z=6 Field Geometry and Configuration Clustering and large scale structure: fields > arcmin (>3-4x correlation length of massive galaxies at z=6) Number of Fields Cosmic variance: 5 fields Field Selection Fields with deep auxiliary data: Extended GOODS-S, Extended GOODS-N, UDS, EGS, COSMOS/UltraVista 3 Epochs, 6 months apart -> variability D1(2h,-4d)) D2 (10h,+2d) (w/COSMOS) D3(14h,+53d) (overlap EGS)) D4(22h,-18d) 16.5x10 GOODS- Size Area IMPACT OF COSMIC VARIANCE (Bright i -drops in four 1 deg 2 CFHTLS; Haojing Yan) D1:D2:D3:D4 ~ 1.2:1.7:1.0:1.8 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* (5 x 10 9 Msun) at z=6 Field Geometry and Configuration Clustering and large scale structure: fields > arcmin (>3-4x correlation length of massive galaxies at z=6) Number of Fields Cosmic variance: 5 fields Field Selection Fields with deep auxiliary data spread in RA (scheduling), DEC (northern, southern terrestrial facilities) 3 Epochs, 6 months apart -> variability SEDS Survey Fields 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* (5 x 10 9 Msun) at z=6 Field Geometry and Configuration Clustering and large scale structure: fields > arcmin (>3-4x correlation length of massive galaxies at z=6) Number of Fields Cosmic variance: 5 fields Field Selection Fields with deep auxiliary data: Extended GOODS-S, Extended GOODS-N, UDS, EGS, COSMOS/UltraVista 3 Epochs, 6 months apart -> variability SEDS: Technical Aspects Expected Number of Sources Sufficient to derive mass functions and perform clustering studies Finlator models: 8000, 2000, and 200 galaxies at z = 5, 6, and 7 few at z ~ 9. Source Selection Initially: Conventional Ly dropout technique Z = 4, 5, 6, and 7: B, V, i, and z Full photo-zs for sample: require matching YJHK data (~26 AB) : UltraVISTA in COSMOS, UKIDSS UDS, 5 yrs To unlock full potential (depth, de-blending): WFC3!!! Area Coverage vs Exposure Time 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 = 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 identified Ly emitters at z = 5 - 7: stellar masses, stellar populations High z counterparts to dwarf galaxies? Different sample compared to dropouts Black hole evolution at z > 6. High-z AGN number counts (constrain evolutionary models) IRAC essential for high-z obscured AGN (z>6: ~100 expected) Relationship to stellar growth Tests of theoretical models of galaxy assembly SED of an i droput Galaxy at z = 6.6 M. Ouchi et al. 2008 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 = 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 identified Ly emitters at z = 5 - 7: stellar masses, stellar populations High z counterparts to dwarf galaxies? Different sample compared to dropouts Black hole evolution at z > 6. High-z AGN number counts (constrain evolutionary models) IRAC essential for high-z obscured AGN (z>6: ~100 expected) Relationship to stellar growth Tests of theoretical models of galaxy assembly Observed SF histories to z~6, test of galaxy models z=7 Labbe+09 z=8 z=6 Dave, Finlator & Oppenheimer 06 Noeske+07 wait for SEDS z=6 Marchesini+09 Evol. of Galaxy Main Sequence Evol. of Stellar Mass Functions Noeske+ 2007b & 2010, in prep. Observed SF History vs Stellar Mass Clustering, abundances: Observed SF History vs Halo Mass Test of Galaxy Formation Models Understand Physics of SF Reionization SEDS: Scientific Objectives Auxiliary Science Galaxy Evolution from z ~ Mass assembly of galaxies: improved stellar masses, photo-zs, etc Emergence of quiescent galaxies (IRAC: quiescent-red vs dust-red) Mid-infrared Variability for AGN Identification A more universal AGN tracer: many variable sources not seen in X-ray Measurement of the Cosmic Infrared Background radiation spatial fluctuations Nature of Infrared Background Fluctuations High-z protogalaxies or faint foreground objects? Project Status, Schedule Warm IRAC performs well First epoch (4h/pointing) UDS observed Next up: COSMOS/UltraVISTA, EGS Total duration: 18 months No proprietary period on raw data After end of observations: release of reduced mosaics, source catalogs Warm 3.6 m Cryo 3.6 m Warm 4.5 m Cryo 4.5 m Warm IRAC Performance: Comparable to Cryogenic UDS Field, 3.6 micron, 1st epoch (4 / 12 h exposure time) SPUDS, 40 min SEDS, 4h AORs: S. Willner, Reduction: M. Ashby UDS, Ch1, 4h AORs: S. Willner Reduction: M. Ashby 5 UDS Field (20 x 20 arcmin) 3.6 micron4.5 micron AORs: S. Willner, Reduction: M. Ashby UDS Field (5 x 5 arcmin) 3.6 micron4.5 micron Frequent worry for deep IRAC exposures: Confusion But: 2/3 of sources are unconfused Summary: Spitzer Warm Mission Exploration Science Program, PI: G. Fazio Unbiased survey at 3.6 and 4.5 microns, 0.9 deg 2 (10x GOODS) 12h/pointing, [3.6] = 26 AB, 5 (0.15 Jy), 2108 hours total Five fields with excellent ancillary data: E-GOODS-N, E-CDFS, EGS, UDS, COSMOS/UltraVISTA Science: First census of galaxy assembly at high z, out to reionization: Stellar mass functions, L* at z=6, high mass end at z=7 Black hole growth at z>6 Clustering -> Galaxy properties as fct. of Halo Mass Star formation histories to z=6 Test and improvement of galaxy and reionization models Nature of LAEs z=1-4 galaxies: photo-zs, stellar populations Nature of IR BG fluctuations Observations underway, 2 epochs, 18 months total, no proprietary period on data Pathfinder for JWST, ALMA, ELTs, radio arrays One of a kind chance to understand the early Universe, very lucky this program got approved. Need WFC3!!!