Table of Contents
Largescale surveys and cosmic structure formation
Forming superclusters (comoving view)
Nongravitational 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 scaledependent antibias in LCDM
Meaning of clustering
Darkmatter 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
PPT Slide
Tiling strategy
The 2dF site
The 2dF facility
2dF on the AAT
Configuring fibres
Data pipeline: realtime Xcorr z’s
PPT Slide
2dFGRS Redshift distribution
Redshift yield
Completeness
Survey mask
Sampling & Uniformity
Cone diagram: 4degree wedge
Fine detail: 2deg NGP slices (1deg steps)
Clustering as f(L): x(r) = (r/r0)g
Measuring bias  1: CMB
Measuring bias  2: Bispectrum
Bispectrum results
PPT Slide
Redshiftspace clustering
? and ?
The CDM power spectrum
Tilt, COBE and cluster normalization
2dFGRS powerspectrum 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
2dFGRS in COLOUR
PPT Slide
PPT Slide
Redshiftspace 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
Summary
