Large-scale surveys and cosmic structure formation


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Table of Contents

Large-scale surveys and cosmic structure formation

Forming superclusters (comoving view)

Non-gravitational caustics

The universe according to CDM

Nonlinear power - discreteness

Nonlinear power - evolution

The CDM clustering problem

Galaxy formation and bias

Bias is inevitable for rare systems

Semianalytic galaxy formation models predict scale-dependent antibias in LCDM

Meaning of clustering

Dark-matter haloes and bias

Correlations from smooth haloes

Halo occupation numbers depend on mass

Results from the 2dF Galaxy Redshift Survey

The 2dFGRS Team

2dFGRS input catalogue

2dFGRS geometry

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Tiling strategy

The 2dF site

The 2dF facility

2dF on the AAT

Configuring fibres

Data pipeline: real-time X-corr zís

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2dFGRS Redshift distribution

Redshift yield


Survey mask

Sampling & Uniformity

Cone diagram: 4-degree wedge

Fine detail: 2-deg NGP slices (1-deg steps)

Clustering as f(L): x(r) = (r/r0)-g

Measuring bias - 1: CMB

Measuring bias - 2: Bispectrum

Bispectrum results

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Redshift-space clustering

? and ?

The CDM power spectrum

Tilt, COBE and cluster normalization

2dFGRS power-spectrum results

Effects of baryons

2dFGRS power spectrum - detail

Power spectrum and survey window

Model fitting

Tests on mock data

Confidence limits

Comparison with other data

Consistency with other constraints

Recovering LCDM

But are you really sure that bias might not depend on scale?

Spectral classification by PCA

LFs by spectral type


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Redshift-space distortions and galaxy type

Power spectrum and galaxy type

Power spectrum: Feb 2001 vs final

Model fits: Feb 2001 vs final

Relation to CMB results

The CMB geometrical degeneracy

2dFGRS + CMB: Flatness

The CMB peak degeneracy

The tensor CMB degeneracy

Detailed constraints for flat models (CMB + 2dFGRS only: no priors)

PPT Slide

Constraining tensors with b


Author: John Peacock