The growth of lss in a dark energy dominated universe
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The Growth of LSS in a Dark Energy Dominated Universe. Marc Davis UC Berkeley. The DEEP2 Galaxy Redshift Survey used the DEIMOS spectrograph at the Keck II telescope to study both galaxy properties and large-scale structure at z~ 1. The DEEP2 Collaboration. Other Institutions

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The growth of lss in a dark energy dominated universe
The Growth of LSS in a Dark Energy Dominated Universe

Marc Davis

UC Berkeley

Texas A&M, May 2007


The deep2 collaboration

The DEEP2 Galaxy Redshift Survey used the DEIMOS spectrograph at the Keck II telescope to study both galaxy properties and large-scale structure at z~1.

The DEEP2 Collaboration

Other Institutions

J. Newman (LBNL)

A. Coil (Arizona)

C. Willmer (Arizona)

B. Weiner (Arizona)

R. Schiavon (UVA)

C. Conroy (Princeton)

N. Kaiser (Hawaii)

D. Finkbeiner

(Harvard)

A. Connolly (Pitt.)

U.C. Santa Cruz

D. Phillips

S. Kassin

K. Noeske

A. Metevier

L. Lin

N. Konidaris

G. Graves

J. Harker

U.C. Berkeley

M. Davis (PI)

D. Croton

M. Cooper

B. Gerke

R. Yan

U.C. Santa Cruz

S. Faber (Co-PI)

D. Koo

P. Guhathakurta


Deep2 has been made possible by deimos a new instrument on keck ii
DEEP2 has been made possible by DEIMOS, a new instrument on Keck II

  • DEIMOS:

  • PI: Faber

  • wide-field multiplexing (up to 160 slitlets over a 16’x4’ field)

  • high resolution (R~5000)

  • spectral range (~2600 Å at highest resolution)

  • CCD array of 8k x 8k

Texas A&M, May 2007



Deep2 mask selection

DEEP2 mask selection Keck II

Targeted galaxies are enclosed with white curves

Solid slits are objects selected on a given mask.

dotted and dashed lines are galaxies from neighboring masks.


Deep2 slitmask spectroscopy
DEEP2 slitmask spectroscopy Keck II

l

position

Using custom-milled slitmasks with DEIMOS we obtained spectra of ~150 targets at a time. A total of 400 slitmasks was required for the survey; we tilted slits up to 30 degrees to obtain rotation curves.

Texas A&M, May 2007


Aegis the a ll wavelength e xtended g roth strip i nternational s urvey

DEEP2/CFHT Keck II

B,R,I

GALEX NUV+FUV

Chandra & XMM:

XMM

Chandra (1.6Ms)

AEGIS:the All-wavelength Extended Groth Strip International Survey

Spitzer MIPS, IRAC

DEEP2 spectra and Caltech/JPL Ks imaging

HST/ACS

V,I (Cycle 13)

Plus VLA (6 & 21 cm), SCUBA, etc….

Texas A&M, May 2007


X ray analysis detection and photometry
X-ray analysis - detection and photometry Keck II

  • P.Nandra et al.

  • Each square has integration time of 200 ksec

  • Source selection and photometry by own method

    • Elliptical shaped PSFs

  • All data will be released in August, 2007

1.6 Ms

Texas A&M, May 2007


A redshift survey at z 1
A Redshift Survey at z=1: Keck II

  • 3 sq. degrees

  • 4 fields (0.5o x <2o)

  • 80 Keck nights, one-hour exposures to RAB=24.1

  • primarily z~0.75-1.4 (pre-selected using BRI photometry)

  • 46,585 unique redshifts, error ~30 km/s

  • ~5·106 h-3Mpc3

  • 1200 l/mm: ~6500-9200 Å

  • 1.0” slit: FWHM 68 km/s

  • z=0.7-1.4 spans lookback time ~6.0 - 8.0 Gyr ago

  • Within DEEP2 we are surveying 2.5 Gyr or ~20% of the history of the Universe, and SDSS/2dF comparisons give ~3x this baseline

Texas A&M, May 2007


Redshift distribution of deep2 survey
Redshift Distribution of DEEP2 Survey Keck II

Texas A&M, May 2007


Deep2 status update
DEEP2 Status Update Keck II

  • DEEP2 began observations in July 2002.

  • Observations are now >95% finished, with >49k spectra in hand and 3 of 4 fields completed.

  • Follow-up observations have begun.

  • First season’s data is already public:

  • http://deep.berkeley.edu/DR1

  • Next data release (DR2) includes ~75% of the data and has also been released! http://deep.berkeley.edu/DR2

Texas A&M, May 2007


Redshift Maps in 4 Fields: z=0.7-1.3 Keck II

Cone diagram of 1/12 of the full DEEP2 sample

Texas A&M, May 2007


Galaxy groups in deep2

position Keck II

l, z

Galaxy groups in DEEP2

  • Overdensities identified in redshift space.

  • Use the VDM algorithm of Marinoni et al. (2002).

  • Group in early DEEP2 data s~250 km/sec

Texas A&M, May 2007


Deep2 group catalog
DEEP2 Group Catalog Keck II

Groups with >350 km/s

Shown are groups for 3 fields

--length of ellipse proportional to velocity dispersion

Texas A&M, May 2007

Gerke et al. 2005,astro-ph/0410721


Real groups mock groups
Real Groups/Mock Groups Keck II

galaxies shown in 3 projections

x-r redshift plot

y-r redshift plot

Real or Mock???

X-y projected on sky

Texas A&M, May 2007


Why search for groups in deep2

  • differences in the volume element varies by 3x between w=0 and w=-1

  • For groups of modest-mass, the evolution of dispersion is 2nd order

Why search for groups in DEEP2?

  • Heavy black curve is T=.3DEIMOS took ~7 years to build; at time of designing science expt. T was still undetermined, and DE was not discussed.



Abundance versus redshift

Abundance versus Redshift Keck II

Simulated Data!!



Dispersion with galaxies
Dispersion with galaxies Keck II

Texas A&M, May 2007


Constraints expected on parameters w, Keck II8, m

Texas A&M, May 2007


Deep2 cluster counts

DEEP2 Cluster Counts Keck II

DEEP2 survey counted ~300 groups

Velocity dispersion measured in each case

Counts of N(, z) is a strong test of w

B. Gerke will have results out “soon”


Conclusions on deep2
Conclusions on DEEP2 Keck II

  • DEEP2 observations are >96% done

  • DR2 has occurred in January:http://deep.berkeley.edu/DR2

  • AEGIS ApJL special issue

  • Way too many new results to cover in one talk!

Texas A&M, May 2007


By combining area with depth aegis allows us to study rare objects in detail
By combining area with depth, AEGIS allows us to study rare objects in detail…

B. Gerke, JN et al. 2006, AEGIS ApJL, Accepted

Texas A&M, May 2007


Like a spectroscopically identified dual agn at z 0 7
Like a spectroscopically identified, dual AGN at objects in detail…z=0.7

Hb

[OIII]

4959

[OIII]

5007

position

l/ z

Texas A&M, May 2007


Hst reveals a fairly normal early type host
HST reveals a fairly-normal early-type host objects in detail…

Texas A&M, May 2007


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