Recent Highlights from the DEEP & AEGIS Surveys David C. Koo - PowerPoint PPT Presentation

Recent Highlights from the DEEP & AEGIS Surveys David C. Koo & DEEP Team UCO/Lick Observatory University of California, Santa Cruz 28 Aug 2007 A Century of Cosmology, Venice, Italy DEIMOS KECK

Outline 1) What’s DEEP? Why useful for cosmology? Status. 2) What’s AEGIS? Why useful ? 3) A few recent science highlights: • New Velocity vs Stellar Mass Relation • Merger rates of Blue & Red Galaxies • Young ? Massive Galaxies at z ~ 0.7 • Panchromatic Study of a HyperLIRG 4) Summary

The DEEP Collaboration UC Berkeley: M. Davis (PI), A. Coil (AZ), C. Conway (Princeton), M. Cooper (AZ), J. Comerford, D. Croton, B. Gerke (KITP), R. Griffith, J. Newman (Pitt), R. Yan (Toronto), UCSC: S. Faber (DEIMOS PI), J. Miller, P. Guhathakurta, D. Koo, J. Cheng, A. Dutton, G. Graves, J. Harker, S. Kassin (Oxford), E. Kirby, N. Konidaris, E. Laird (London), L. Lin (N. Taiwan U.), J. Lotz (AZ), A. Metevier (Sonoma), K. Noeske (Harvard), A. Phillips , D. Rosario, K. Rubin, B . Weiner (AZ), C. Willmer (AZ), Associates & AEGIS: K. Bundy(Toronto), S. Chapman (Caltech), A. Connolly (Pitt), C. Conselice (Nottingham-UK), P. Eisenhardt (JPL), D. Finkbeiner (SDSS), J. Gallego (UCM), R. Guzman(UFl), C. Hoyos (UFl), R. Ivison (Edinb), M. Hudson (Waterloo), N. Kaiser (HI), G. Luppino(HI), J. Lowenthal (Smith), C. Martin (UCSB), L. Moustakas (JPL), L. Parker (ESO), F. Prada & N. Rodriquez (Granada), V. Sarajedini (Ufl), R. Schiavon (UVa), L. Simard (HIA), V. Villar(UCM), G. Wirth (Keck), & Spitzer IRAC MIPS GTO, GALEX, Keck, & Chandra Teams Supported by: NSF, NASA, UCO/Lick, CARA, Sun, Quantum

DEEP’s DEEPs • DEEP: Deep Extragalactic Evolutionary Probe (initiated by CfPA 1991) • DEEP1: Pilot Survey for DEEP2 & DEEP3, 1995-2001 • Keck spectra (1st generation instruments) & HST images (V & I) • Targets: Groth Survey Strip (GSS) & Selected Area 68 • Redshifts: 600 in GSS to I~23.5 at z = 0.2 to 3.0 • Science: Kinematics, structure, luminosity & colors, abundances, SFR, etc. • DEEP2: Main Survey (1 H): 80 Keck nights, 2002-2005 • Keck spectra : DEIMOS , Resolution ( λ / Δλ ) = 5000 & CFHT images (BRI) • Targets: 3 fields 0.5x2 deg & Special one of 0.25x2 deg Extended Groth Strip (EGS) with Spitzer, GALEX, VLA, Chandra, CFHT Legacy, & others • Redshifts: 40,000 to R = 24.1; except EGS , uses photo-z for z = 0.7 - 1.4 • Science: DEEP1 + clustering, environment, densities, lensing, etc. • DEEP3: Follow-up Surveys : ??? Keck nights, 2003-2010 • Bluer & deeper spectra R ~ 2500 in EGS, GOODS-N, GOODS-S • Follow-up spectra of special subsamples: e.g., X-ray, Spitzer sources • Near-IR spectroscopy with Adaptive Optics & Integral Field Units

Las Campanas Redshift Survey vs DEEP2 Z ~ 1.5 ~9 Gyr MIRROR: 2.5m vs 10m NUMBER: ~26K vs ~35K MEDIAN Z: ~0.1 vs ~0.9 Z ~ 0.7 DEPTH: R < 18 vs ~ 24 ~6 Gyr RES (km/s): >300 vs ~70 FINISHED: 1995 vs 2007

CFHT (Images) Hubble (Optical) KECK (Spectra) SPITZER (IR) Extended GALEX (UV) Groth Strip VLA (Radio) CHANDRA (X-ray)

http://aegis.ucolick.org

AEGIS SURVEYS very deep

Why use DEEP for Cosmological & Multiwavelength Studies ? 1) VERY FAINT R ~ 24: reaches redshifts z ~ 1+ where a lot of action exists: • dark energy overtakes gravity; • major transition for star formation & AGN ; • galaxies assembling and converging on their present day structure and morphology; • Many counterparts expected & detectable with current very deep to deepest X-ray, far- UV, mid to far IR, & radio surveys.

Why use DEEP for Cosmological & Multiwavelength Studies ? 2) LARGE NUMBERS: allows studies • of large scale structure ; • of rarer targets expected from X-ray to radio (e.g, ULIRGs & AGN); • of diverse environments (close pairs, groups, clusters); and • of stacked data of special subsets for reaching ultra-deep limits (e.g. Radio signal of non-AGN)

Why use DEEP for Cosmological and Multiwavelength Studies? 3) HIGH SPECTRAL RESOLUTION (~ 30km/s) • internal kinematics that give dynamical masses that can be surrogates for halo virial masses and compared to stellar masses (e.g. from IRAC on Spitzer); • provide kinematic signatures of mergers, which play a major role in galaxy assembly, starbursts, and AGNs; • Detects and measures of low inter-galaxy velocities for studies of halos and small groups & environment; • Yields spectral line profile shape , due, e.g. to flow velocities, & tests of time variation of the fine structure constant

Why use DEEP for Cosmological & Multi-Wavelength Studies? 4) HIGH S/N SPECTRA: provides: • Better survey completeness in both total number and surface density on the sky; • rich suite of spectral line data that complement key measures from other wavelength surveys: star formation (OII vs Ha in NIR, X-ray, FUV, FIR, submm, radio), metallicity (O/H, Fe/H vs IRAC colors and dust), and age (e.g., vs dust from Spitzer & rest FUV upturn from NUV from GALEX)

DEEP2 STATUS (28 August 2007) 1) DEIMOS was commissioned in mid-2002 and is FULLY OPERATIONAL 2) DEEP2 1HS: First Light in JULY 2002 DEEP3 Some data in GOODS-N, GOODS-S, & EGS 3) Keck NIGHTS: 92 from Fall 2002 to Spring 2007 4) REDSHIFTS: DEEP2: ~35K spectra = 90% done 2002 Fall data (10%): 5K z’s (DR1 Nov 2004) All DEEP2 except EGS: 25K z’s (DR2 Jan 2007) All DEEP2 through 2005: 35K z’s (DR3 Aug 2007) 5) DEEP3 approved for ~25 DEIMOS Keck nights over 3- 4 years: finish orig. EGS; go fainter; X-ray & Spitzer sources DEEP2 ARCHIVE: http://deep.berkeley.edu/

Redshift vs Luminosity R~24 Galaxies exist in large I~24 numbers beyond z = 1 R~24 # L > L* I~22.5 & z > 1 L *

Four Highlights from DEEP2 Since its inception, DEEP1 and DEEP2 have produced about 60 refereed papers in topics ranging from large scale structure, groups, and correlation functions; the nature and evolution in the structure, chemical abundances, star formation rates, environments, and kinematics of various subsets of galaxies and their subcomponents; the luminosity, stellar mass, star formation and merger functions for galaxies; and the evolution of infrared bright galaxies and AGNs. DEEP is an on-going project. The following are recent examples to highlight the range of science only possible with DEEP2’s spectral resolution and large sample size.

Dramatic Reduction in Scatter with use of new Kinematic Measure: S = √ 0.5 V rot 2 + σ 2 M*: stellar mass uses IRAC Morphology: J. Lotz’s M20 & Gini Kassin et al (2007) Weiner et al (2006)

Pair Fraction Averaged No. Companions per Galaxy vs Redshift Using DEEP2 sample of 21,500 galaxies, and kinematic selection of over 500 pairs with velocity difference of < 500 km/s: Best fit to (1+z) m yields m ~ 0.36+-0.21, which is consistent with almost no evolution from Lin et al. (2004). Rising line shows m~ 3 claimed by other groups. Blue: deep2; Lin et al. 07, in prep. red: TKRS; Lin et al. 2007 Redshift green: MGC+CNOC2

Co-moving Merger Rates from DEEP2 Lin et al. 07, in prep. Co-moving Merger Rate Mergers/Mpc 3 /Gyr • at z~0.8: Blue mergers : Red mergers: Blue-Red mergers ~ 6 : 1 : 2 • the red mergers (dry mergers) becomes more important at lower z But integrated rate is still low at about 0.15 for L* galaxies since redshift z~1.

Near Perfect Match to the Predictions of Khochar and Burkert 2003

Metal-Poor Massive Galaxies discovered at z ~ 0.7 using [OIII] 4363A (“Gold Standard” for O/H metallicity): Youngest Massive Galaxies? Hoyos et al 2007

CXO-J141741.9+522823 MIPS 24 µ m ACS Chandra AGN z=1.15 Galaxy evolution with Spitzer and Herschel, June 1 st , 2006

CXO-J141741.9+522823 Far-IR Mid-IR References Nandra+05 Barmby+06 Optical Sub-mm Ashby+06 Higdon+04 Eales+00 Webb+03  Fomalont+91 Chapman+05 Radio 4.5 10 12 4.5 10 12 X-ray (1-3 10 12 L ) AGN Starburst  LeFloch et al. 2007

Summary • DEEP2 & AEGIS provide powerful surveys to study cosmology and galaxy & AGN evolution with: 1) solid access to z ~ 1, 2) large numbers, 3) star formation rates, 4) metallicities, 5) Ages, 6) stellar and dynamical Masses, & 7) environment • Some science highlights near z ~ 1 include: • Discovery and use of a new “total” kinematic measure that shows little evolution and scatter to redshifts z ~ 1. • Merger rates for dry-dry and dry-wet increase with time while wet- wet decline, but all are at relatively low rates. • Discovery of a rare class of very low-metallicity but luminous galaxies with high mass. Are these recent counterpart to z ~ 3 galaxies? • Re-discovery of a very rare Hyper LIRG at z ~ 1.15 that shows equal star formation and AGN luminosities and thus support for co- evolution growth of SMBH and spheroid.