The Spitzer Extended Deep Survey SEDS Spitzer Warm

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, Cf. A – 47 Co-I’s 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 σ) – 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 Cf. A: University of Chicago/KICP: Brant Robertson Lars Hernquist, Matt Ashby, Jiasheng Huang, Kai Noeske, Steve Willner, Stijn Wuyts, T. J. Cox, Yuexing Li, Kamson Lai Swinburne University: Darren Croton Max-Planck-Institut für Astronomie: University of Florida, Gainesville: Vicki Sarajedini Hans-Walter Rix, Eric Bell, Arjen van der Wel Astrophysikalisches Institut, Potsdam: University of Califronia, Santa Cruz: Andrea Cattaneo Sandy Faber, David Koo, Raja Guhathakurta, Garth Illingworth, Rychard Bouwens University of Massachusetts, Amherst: NASA/GSFC: Royal Observatory Edinburgh: Sasha Kashlinsky, Rick Arendt, John Mather, Harvey Moseley James Dunlop Carnegie Observatories: Haojin Yan, Ivo Labbe, Masami Ouchi University of Pittsburgh: Jeff Newman Stanford University/KIPAC: Risa Wechsler Hojun Mo Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan: Lihwai Lin National Research Council, Herzberg Institute of Astrophysics: Luc Simard Space Telescope Science Institute: Anton Koekemoer Texas A&M University: Casey Papovich University of Arizona: Ben Weiner, Romeel Dave, Kristian Finlator, Eiichi Egami University of Western Ontario: Pauline Barmby Imperial College, London: Kirpal Nandra Tohoku University, Japan: Toru Yamada Oxford University: Dimitra Rigopoulou University of California, Riverside: Gillian Wilson

SEDS: The Spitzer Extended Deep Survey - Motivation • Only Spitzer can see redward of 4000 A 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 σ (0. 15 μJy) – Robustly measure M* (5 x 109 Msun) at z=6 • Field Geometry and Configuration – Clustering and large scale structure: fields > 20 - 30 arcmin – (>3 -4 x 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/Ultra. Vista 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 σ (0. 15 μJy) – Robustly measure M* (5 x 109 Msun) at z=6 • Field Geometry and Configuration – Clustering and large scale structure: fields > 20 - 30 arcmin – (>3 -4 x 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/Ultra. Vista 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 σ (0. 15 μJy) – Robustly measure M* (5 x 109 Msun) at z=6 • Field Geometry and Configuration – Clustering and large scale structure: fields > 20 - 30 arcmin – (>3 -4 x 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/Ultra. Vista 3 Epochs, 6 months apart -> variability

IMPACT OF COSMIC VARIANCE (Bright i′ -drops in four 1 deg 2 CFHTLS; Haojing Yan) D 1(2 h, -4 d)) D 2 (10 h, +2 d) (w/COSMOS) D 4(22 h, -18 d) D 3(14 h, +53 d) (overlap EGS)) 16. 5’x 10’ GOODSSize Area D 1: D 2: D 3: D 4 ~ 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 σ (0. 15 μJy) – Robustly measure M* (5 x 109 Msun) at z=6 • Field Geometry and Configuration – Clustering and large scale structure: fields > 20 - 30 arcmin – (>3 -4 x 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 σ (0. 15 μJy) – Robustly measure M* (5 x 109 Msun) at z=6 • Field Geometry and Configuration – Clustering and large scale structure: fields > 20 - 30 arcmin – (>3 -4 x 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/Ultra. Vista 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 Lyman dropout technique • Z = 4, 5, 6, and 7: B, V, i, and z – Full photo-zs for sample: require matching YJHK data (~26 AB) : Ultra. VISTA in COSMOS, UKIDSS UDS, 5 yrs – To unlock full potential (depth, de-blending): WFC 3!!!

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 = 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 identified Lyα 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 = 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 identified Lyα 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 Evol. of Galaxy Main Sequence Noeske+07 Labbe+09 z=6 Marchesini+09 wait for SEDS • Test of Galaxy Formation Observed SF History vs Stellar Mass Models • Understand Physics of SF • Reionization z=8 z=6 Dave, Finlator & Oppenheimer 06 Evol. of Stellar Mass Functions Clustering, abundances: “Observed” SF History vs Halo Mass Noeske+ 2007 b & 2010, in prep.

SEDS: Scientific Objectives • Auxiliary Science – Galaxy Evolution from z ~ 1 - 4 • 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 (4 h/pointing) UDS observed • Next up: COSMOS/Ultra. VISTA, EGS • Total duration: 18 months • No proprietary period on raw data • After end of observations: release of reduced mosaics, source catalogs

Warm IRAC Performance: Comparable to Cryogenic Warm 3. 6 μm Cryo 3. 6 μm Warm 4. 5 μm Cryo 4. 5 μm

UDS, Ch 1, 4 h AORs: S. Willner Reduction: M. Ashby

5 UDS Field (20 x 20 arcmin) 3. 6 micron 4. 5 micron AORs: S. Willner, Reduction: M. Ashby

UDS Field (5 x 5 arcmin) 3. 6 micron 4. 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 (10 x GOODS) 12 h/pointing, [3. 6] = 26 AB, 5 σ (0. 15 μJy), 2108 hours total Five fields with excellent ancillary data: – E-GOODS-N, E-CDFS, EGS, UDS, COSMOS/Ultra. VISTA • 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