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The WiggleZ Dark Energy Survey. Michael Drinkwater for the team Australia : Blake, Brough, Colless, Couch, Croom, Davis, Glazebrook, Jelliffe, Jurek, Li, Pimbblet, Poole, Pracy, Sharp, Wisniosiki U.S.A. : Foster, Gladders, Madore, Martin, Small, Wyder Canada : Gilbank, Woods, Yee.

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The wigglez dark energy survey

The WiggleZ Dark Energy Survey

Michael Drinkwater for the team

Australia: Blake, Brough, Colless, Couch, Croom, Davis, Glazebrook, Jelliffe, Jurek, Li, Pimbblet, Poole, Pracy, Sharp, Wisniosiki

U.S.A.: Foster, Gladders, Madore, Martin, Small, Wyder

Canada: Gilbank, Woods, Yee

Motivation

Design & Progress

Large Scale Structure Results

Other Results

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1 motivation
1. Motivation

  • Need to sample around redshift z=0.6 when acceleration starts

  • Survey aims:

    • Measure BAO scale to 2% in a sample of 240,000 galaxies at 0.3<z<0.9

    • Measure w to 10% to independently validate constant dark energy model

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Motivation
Motivation

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2 design progress
2. Design & Progress

  • GALEX satellite imaging

    • UV-selected galaxies

    • Medium Imaging Survey extended

    • NUV < 22.8

  • Optical imaging: r < 22.5

    • SDSS (North)

    • RCS2 survey on CFHT (South)

  • AAT’s new AAOmega fibre spectrograph

    • 220-night large project

    • Measure 240,000 redshifts

    • Star forming galaxies

    • Emission line redshifts in short 1-hour exposures

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Example spectra
Example spectra

Quality = 5 (high)

Redshift z=0.57

R = 21.4 mag

Quality = 3 (acceptable)

Redshift z=0.86

R = 21.2 mag

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Survey coverage
Survey coverage

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Design improvements
Design Improvements

  • New spectrograph beam splitter

    • Moved spectra 100 nm to the red

    • More reliable redshifts

  • Optical Colour Selection

    • Increased median redshift to zmed=0.6

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Survey status
Survey Status

Galaxies in the 15-hour WiggleZ field… to 3.3 Gpc distance

  • Progress

    • Observations ¾ done

    • Scheduled to run 2006 to 2010 August

    • Over 140,000 galaxies measured

    • Have doubled the number of known z>0.5 galaxies from the two largest existing surveys (DEEP2 & VIMOS)

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3 large scale clustering results
3. Large scale clustering results

The 2dF control system…

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Wigglez power spectrum
WiggleZ power spectrum

Linear model is

good fit to k = 0.3

5% accuracy in

dk = 0.01 bins

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By Chris Blake


Wigglez power spectrum1
WiggleZ power spectrum

Divided by reference model with BAO signal removed.

Model divided by reference

Model convolved with survey window

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By Chris Blake


Cosmological parameters
Cosmological Parameters

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By Chris Blake


Predicted final sensitivity
Predicted final sensitivity

Predicted precision in measurement of (wconst, ΩM) combined with supernovae

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By Tamara Davis


4 other results
4. Other results

  • Small scale clustering (Blake et al. 2009)

  • UV luminosity function (Russell Jurek’s PhD)

  • Growth of structure (Carlos Contreras’ PhD)

  • Super starburst galaxies (Emily Wisnioski’s PhD)

  • Future work

    • Neutrino mass

    • Galaxy bispectrum

    • Genus statistic

    • Homogeneity scale of Universe (vs LTB models)

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Small scale clustering
Small scale clustering

Unity of the Universe

By Chris Blake


Small scale clustering1
Small scale clustering

Unity of the Universe

By Chris Blake


The uv galaxy luminosity function
The UV galaxy luminosity function

Russell Jurek’s PhD

First ever sample of bright end of UV luminosity function

WiggleZ

N=47,747

N=9356 (photo-z)

N=1869

N=1039

N=2976

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Uv contribution to star formation
UV contribution to star formation

MNUV

-18 -20 -22

0.01 0.02 0.03

Fraction of universal star formation density

  • WiggleZ galaxies have the highest SF at any redshift

  • Their contribution peaks at z≈0.6

0.2 0.6 1.0

redshift (z)

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Russell Jurek’s PhD


Growth of structure
Growth of structure

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Super starburst galaxies
Super starburst galaxies

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Neutrino mass
Neutrino Mass

  • Advantage of WiggleZ

    • Galaxies less strongly clustered than LRGs

    • Higher redshift

  • Better power spectrum measurement

    • Have many more Fourier scales before it goes non linear

Non-linear growth

of structure

Unity of the Universe

By Chris Blake


Summary

The technology behind WiggleZ: 2dF positioning fibres on the AAT

Summary

  • Aims of WiggleZ

    • Survey the largest ever volume of the z>0.5 Universe

    • 240,000 galaxies in 1 Gpc3

    • Measure BAO scale to 2%

    • Measure constant w to 10%

  • BAO not measured until observations finish 2010 May

  • Many other science applications

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2df on a bad day
2dF on a bad day AAT

Note the special error message: “Too many errors.”

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