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The 2Df Galaxy Redshift Survey and Cosmological Simulations Carlos S University of Durham The 2dF galaxy redshift survey and cosmological simulations Carlos S. Frenk Institute for Computational Cosmology, Durham Institute for Computational Cosmology The 2dF Galaxy Redshift University of Durham Survey 1997- 2002 250 nights at 4m AAT 221,000 redshifts to bj<19.45 median z = 0.11 First 100k z's released June/01 Full catalogue released July/03 Institute for Computational Cosmology 2dF Galaxy Redshift Survey: University of Durham Team Members Ivan K. Baldry10 Carlton M. Baugh2 Joss Bland-Hawthorn1 Terry Bridges1 Russell Cannon1 Shaun Cole2 Matthew Colless3 Chris Collins13 Warrick Couch5 Nicholas Cross6 Gavin Dalton9 Kathryn Deely5 Roberto De Propris5 Simon P. Driver6 George Efstathiou8 Richard S. Ellis7 Carlos S. Frenk2 Karl Glazebrook10 Edward Hawkins12 Carole Jackson3 Ofer Lahav8 Ian Lewis9 Stuart Lumsden11 Steve Maddox12 Darren Madgwick8 Stephen Moody8 Peder Norberg2 John A. Peacock4 Will Precival4 Bruce A. Peterson3 Mark Seaborne9 Will Sutherland4 Keith Taylor7 Institutions 1Anglo-Australian Observatory 2University of Durham 3The Australian National University 4University of Edinburgh 5University of New South Wales 6University of St Andrews 7California Institute of Technology 8University of Cambridge 9University of Oxford 10Johns Hopkins University 33 people at 11University of Leeds 12University of Nottingham 13 Liverpool John Moores University 12 Institute for Computational Cosmology institutions The 2dF galaxy redshift survey University of Durham QuickTimeã and a YUV420 codec decompressor are needed to see this picture. Institute for Computational Cosmology The 2dF galaxy redshift survey University of Durham 221414 galaxies ) k ( P Galaxy power spectrum 3 k g in redshift space, o L convolved with survey 2dF power spectrum 100k window, inclunding non- release linear effects Percival etal 01 Institute for ComLputoatgion alk C o(smho loMpgy c-1) Galaxy surveys and University of Durham cosmological simulations Simulations are essential for: • Taking into account window function and selection effects • Taking into account non-linear effects and `galaxy bias' • Assessing systematic and random errors • Comparing data to theory Simulations must: • Be realistic • Have a sufficiently large volume • Resolve the structures of interest ⇒ Large number of particles Institute for Computational Cosmology ΛCDM Hubble Volume Simulation Hubble Volume N-body simulatn Ω Ω Λ=0.7; m=0.3 σ h=0.7; 8=0.9 9 Np= 10 L = 3000 Mpc 12 mp = 1x10 Mo Virgo consortium (1999) 3000 Mpc/h Real and simulated 2dF galaxy survey University of Durham Real Simulated Institute for Computational Cosmology The Millennium simulation University of Durham Cosmological N-body simulation · 10 billion particles · 500 h-1 Mpc box × 8 -1 · mp = 8 10 h Mo UK, Germany, Canada, US Ω Ω Ω collaboration · =1; m=0.25; b=0.045; σ h=0.73; n=1; 8 =0.9 Simulation data available at: × 6 20 10 gals brighter than LMC http://www.mpa-garching.mpg.de/Virgo · Carried out at Garching using Pictures and movies available at: L-Gadget by V. Springel www.durham.ac.uk/virgo (27 Tbytes of data) Institute for Computational Cosmology QuickTimeã and a 3ivx D4 4.5.1 decompressor are needed to see this picture. The mass power spectrum University of Durham The non-linear mass power spectrum is accurately determined by the Millennium simulation ) ªbaryon wigglesº k over large range of ( 2 scales ∆ linear theory k [h/Mpc] Institute for Computational Cosmology CMB anistropies and large-scale structure University of Durham 2dFgrs Institute for Computational Cosmology Baryon oscillations in the power spectrum University of Durham • Predicted by CDM model Ω Ω • Can be used to estimate b/ m • Provide a ªstandard rulerº that can be used to measure w First tentative detection in 100k 2dFGRS Institute for Computational Cosmology 100k 2dFGRS power spectrum University of Durham 2dFGRS PS divided by Ωh=0.25 CDM model (zero baryons) 120k redshifts Percival etal 2001 Institute for Computational Cosmology Baryon oscillations in the power spectrum University of Durham Oscillations difficult to detect because: • Amplitude is very small • Survey window can smooth over features • Non-linear effects can erase oscillations • Wiggles are in mass, but we observe galaxies (in z-space) Need to use large cosmological simulations to establish detectability of baryon oscillations. Institute for Computational Cosmology University of Durham Baryon oscillations Baryon oscillations are predicted in the dark matter P(k) in linear theory: 1. Are they erased by non-linear evolution? 2. Are they also present in the galaxy distribution? Institute for Computational Cosmology The mass power spectrum University of Durham Millennium simulation z=127 The Millennium sim is large Simulation k enough to resolve / ) baryonic wiggles k ( in the matter 2 Linear theory power spectrum ∆ Virgo consortium Springel etal `05 k (h/Mpc)Institute for Computational Cosmology The mass power spectrum University of Durham Millennium simulation z=16 k / ) k ( 2 ∆ Virgo consortium Springel etal `05 k (h/Mpc)Institute for Computational Cosmology The mass power spectrum University of Durham Millennium simulation z=5 k / ) k ( 2 ∆ Virgo consortium Springel etal `05 k (h/Mpc)Institute for Computational Cosmology The mass power spectrum University of Durham Millennium simulation z=0.8 Non-linear evolution k / accelerates the ) k ( growth of power 2 and eliminates ∆ structure in the spectrum by mode-coupling Virgo consortium Springel etal `05 k (h/Mpc)Institute for Computational Cosmology The mass power spectrum University of Durham Millennium simulation z=0 Non-linear evolution k / accelerates the ) k ( growth of power 2 and eliminates ∆ structure in the spectrum by mode-coupling Virgo consortium Springel etal `05 k (h/Mpc)Institute for Computational Cosmology Baryonic wiggles in the power spectrum University of Durham Baryonic oscillations in the dark matter PS survive non-linear effects for log k ≤ -0.7 What about in the galaxy PS? Institute for Computational Cosmology z = 0 Dark Matter University of Durham Populating the MS with galaxies Semi-analytic modelling • Find dark matter halos • Construct halo merger trees • Apply SA model (gas cooling, star formation, feedback) Springel etal 04 Institute for Computational Cosmology z = 0 Galaxy light University of Durham Crotton etal 05 Institute for Computational Cosmology University of Durham 14 10 Mo Dark matter Galaxies Institute for Computational Cosmology Baryon wiggles in the galaxy distribution Power spectrum from MS divided by a baryon-free ΛCDM spectrum z=7 z=3 Galaxy samples DM gals matched to plausible large observational surveys at given z z=1 z=0 Springel et al 2004 The final 2dFGRS power spectrum University of Durham 2dFGRS 221,000 z's Covariance matrix computed from mock catalogues Cole, Percival, Peacock + 2dFGRS `05 Institute for Computational Cosmology The final 2dFGRS power spectrum University of Durham Ω P(k) / Pref( baryon=0) Baryon oscillations conclusively Λ detected in CDM model 2dFGRS!!! Demonstrates that structure grew by gravitational instability in ΛCDM ΛCDM convolved universe with window Cole + 2dFGRS `05 Institute for Computational Cosmology The final 2dFGRS power spectrum: University of Durham parameter estimation · Shape of P(K) depends on Ωh · Oscillations depend Ω Ω on b/ m · Amplitude depends σ gal on 8 Ωh = 0.161 ± 0.015 Ω Ω ± b/ m = 0.194 0.045 σ gal ± 8 (L*) = 0.870 0.029 Cole + 2dFGRS `05 Institute for Computational Cosmology Cosmological parameters: CMB + University of Durham 2dF Ω Ω Ω σ gal The 2dF power spectrum depends on mh, b / m, 8 , fν, ¼ The CMB power spectrum depends on , , w , w , f , w ,t , n , n , A ,r , b k L b dm DE s t s Combining 2dF and CMB breaks parameter degeneracies Institute for Computational Cosmology 2dFGRS + CMB: flatness University of Durham BoomePrraen-gW, DMASIA,P Maxma, CBI CMB alone has a geometrical degeneracy: large curvature is not ruled out Adding 2dFGRS power spectrum forces flatness: Ω | 1 - tot | < 0.04 2dFGRS 100k Efstathiou + 2dFGRS team MNRAS 330, L29 (2002) Institute for Computational Cosmology Spergel etal `03 University of Durham The Guardian Dec/19/2003 Institute for Computational Cosmology University of Durham Cosmological parameters Pë , , w , w , f , w ,t , n , n , A ,r ,b k L b d m DE s t s Data: • CMB → WMAP, CBI, ACBAR and VSA • LSS → Full 2dFGRS Method: • MCMC • Use halo Model to relate distribution of galaxies to distribution of mass (galaxy bias) Sanchez, Padilla, Baugh `05 Institute for Computational Cosmology Parameter constraints University of Durham Pë , , w , w ,t , n , A k L b d m s s CMB only¼ CMB + 2dF¼ Λ Λ Ω Ω Ω Ω k k Sanchez etal `05 Institute for Computational Cosmology Parameter constraints University of Durham Pë , , w , w ,t , n , A k L b d m s s CMB only¼ CMB + 2dF¼ h h Ω Λ ΩΛ Sanchez etal `05 Institute for Computational Cosmology Effect of neutrinos University of Durham Free-stream length: 80 -1 (Σ mν /eV) Mpc Ων=0.05 Ω 2 Σ ( m h = mν / 93.5 eV) Σmν ~ 1 eV causes lower power at almost all scales, or a bump at the largest scales 100k 2dFGRS Σ mν < 1.8 ev Eleroy + 2dFGRS team `02 Institute for Computational Cosmology Parameter constraints University of Durham Pë , w , w ,f ,t , n , A L b dm s s CMB only¼ CMB + 2dF¼ ν ν f f n s ns Σ marginalizing mν < 1.1 ev (95% c.l.) Institute for Computational Cosmology Parameter estimation University of Durham CMB + 2dFGRS Ωm = 0.224 ± 0.024 Data: Ωb = 0.055 ± 0.007 → Ω ± • CMB WMAP, CBI, k = -0.034 0.018 ACBAR and VSA ΩΛ = 0.809 ± 0.037
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