The 2dF Galaxy Redshift Survey
Overview and Results

30 June 2003

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Table of Contents
 
  1. The 2dF Galaxy Redshift Survey
  2. The 2dFGRS team
  3. Effective sizes of z-surveys
  4. The 2dF facility
  5. 2dF on the AAT - side view
  6. 2dF on the AAT - top view
  7. Focal plane and fibre positioner
  8. The APM Galaxy Survey
  9. 2dFGRS survey design
  10. Survey magnitude limit mask
  11. Redshifts
  12. Final status of survey observations
  13. Sky coverage and N(z)
  14. Completeness mask
  15. Completeness
  16. Cone diagram: 3-degree slice
  17. Fine detail: 2-deg NGP slices (1-deg steps)
  18. Structure + cosmology highlights
  19. Power spectrum comparison
  20. The CDM power spectrum
  21. Effect of baryons on P(k)
  22. The galaxy power spectrum
  23. Fits to the power spectrum
  24. The shape parameter and the baryon fraction - I
  25. The shape parameter and the baryon fraction - II
  26. Redshift-space distortions
  27. Redshift-space correlation function
  28. Measuring bias I. - 2dFGRS + CMB
  29. Measuring bias II. - The bispectrum
  30. Cosmology from 2dFGRS + CMB
  31. 2dFGRS+CMB fits - flat cosmology
  32. 2dFGRS+CMB fits - general
  1. The CMB power spectrum
  2. Comparison to WMAP
  3. Constraints on the neutrino mass
  4. The dark energy equation of state
  5. Galaxy luminosity function
  6. LF comparisons - I
  7. LF comparisons - II
  8. Bivariate brightness distribution
  9. NIR luminosity function and stellar mass function
  10. Correlation function in redshift space
  11. Variation of clustering/bias with luminosity
  12. Spectral classification by PCA
  13. Luminosity functions by spectral type
  14. Colours and spectral types
  15. Distribution of non-star-forming galaxies
  16. Distribution of star-forming galaxies
  17. Power spectrum & galaxy type - I
  18. Power spectrum & galaxy type - II
  19. Power spectrum & galaxy type - III
  20. Redshift-space distortions and galaxy type
  21. Spectral types in clusters
  22. Luminosity function of cluster galaxies
  23. LF variation with cluster properties
  24. LFs for different spectral types
  25. Field vs cluster LFs by type
  26. Trends with spectral type
  27. Closed box model
  28. A better model?
  29. SFR vs environment in clusters
  30. Star-formation history
  31. Groups and clusters
  32. The 2dF Galaxy Redshift Survey

Matthew Colless, colless@mso.anu.edu.au,