Cosmology from Large Scale Structure Surveys Changbom Park Feb. 27, 2008 School of Physics Korea Institute for Advanced Study

A sketch of Astronomer's methods to measure cosmological parameters (DE's w)

『What we want to know』 1. Spacetime 2. Matter 3. Phenomena/Laws Homogeneous & isotropic space Geometry & topology of space (flat & infinite?) Expansion of space ( matter) Past and future of the Universe (why now?) 2. Matter Contents and nature (what & how much) Primordial fluctuation () Structure formation (when & how, environment) 3. Phenomena/Laws

the Uni-verse: a map of our play-ground

1. Recombination & Decoupling Dark First NL Evolution LSS hear & now age structures of galaxies 1. Recombination & Decoupling  CMB radiation. Let there be primeval light ! 2. Dark Age  What is buried here? 2. First structures & Reionization  Let there be star light ! 4. High-z objects and Evolution of galaxies  Quasars, Ly-a forest clouds 5. Large-scale structure and nearby objects  Cosmic zoo: clusters, voids, filaments & walls of galaxies Recent events in the universe

Expansion of space & Growth of structures Ideas to draw information on the universe 1. Look at primordial fluctuations directly CMB (+neutrino, gravitational wave) => geometry of space, matter contents, matter P(k), non-Gaussianity 3. Study the expansion history of the space : H(t) or r(z) use standard candle (SN Ia), rulers (BAO, topology) => matter contents (DE w) 4. Measure the growth of structures use gravitational lensing, cluster abundance depends on expansion of space, matter power spectrum 5. Study the properties of non-linear structures properties of galaxies, clusters Expansion of space & Growth of structures

Cosmic microwave background anisotropy: CMB anisotropy: Primordial & ISW Cosmic microwave background anisotropy: geometry of space, matter contents, matter P(k), non-Gaussianity only at z~1100, 2d map, foregrounds

WMAP Experiment WMAP Observatory Launched on 30 June 2001 to L2 of Sun-Earth system 1.4m*1.6m primary + 10 feed horns in each 2 focal plane Bands 1 K 1 Ka 2 Q 2 V 4 W Ν [GHz] 22.8 33 40.7 60.8 93.5 FWHM [°] 0.82 0.62 0.49 0.33 0.21

Observed ΔT Maps W 94GHz 0.21° V 61GHz 0.33° Q 41GHz 0.49° K 23GHz 0.82° Ka 33GHz 0.62° Galactic emission + CMBR + others

WMAP's 3 year Map Park, Park, Gott (2007)

Spergel et al. (2007) 3yr & 1yr data 3yr & 1yr fits

Shape of T Power Spectrum Super-horizon scale fluc. SW effect 1∼0.1rH fluc. with initially coherent phases Oscillation & Doppler effect Radial averaging & radiation diffusion

Spergel et al. (2007) 3yr & 1yr constraints

Park, Park, Gott (2007)

HI HI HI HI HI HI HI HI HI HI HI HI HI HI HI HI 3D HI distribution & reionization

3D HI distribution : 21cm tomography mapping most of our observable universe Power spectrum of 21cm fluctuations HI HI HI HI HI HI HI HI HI HI HI HI HI HI Bright in HI !

Gravitational Lensing: Strong & Weak only projected mass along the line of sight

Shear map expected in SCDM Jain, Seljak & White (2000) mass fluctuations along the line of sight -->Weak lensing by LSS --> coherent distortions in the observed shapes of background galaxies Shear map expected in SCDM

CFTHLS weak-lensing survey: i<24.5 & 22 deg2 Spergel (2007)

Type Ia Super Novae Intrinsic dispersion, systematics

r(z) relation : Expansion history SN Ia as a standard candle Transition from deceleration to acceleration at z= 0.46 ± 0.13 (Riess et al. 2004)

μ = m-M = 5log dl + 25 Ωm=0.27, ΩΛ=0.73 Riess et al. (2007)

Matter contents Dark energy Ωm=0.29±0.050.03, ΩΛ=0.71 (if flat U) (Riess et al. 2004) (Riess et al. 1998) (Riess et al. 2004) Matter contents Ωm=0.29±0.050.03, ΩΛ=0.71 (if flat U) Dark energy w = -1.02±0.130.19, w<-0.76 at 95% (if P=wρc2)

Clusters

Clusters of galaxies Searched by X-ray, SZ effect abundance d2N/dMdz spatial distribution P(k)

Future experiments clusters CMB SN Ia

Large Scale Structure in linear ~ quasi-linear regime : P(k), BAO, Topology

Geometric methods using the large scale structures Standard rulers (Actual objects or Features in PS/CF)  measure Δz & Δθ  H(z)DA(z)  Ωm, ΩΛ, w (=dt/a) r|| r┴ (=r dθ) where H(z)

BAO (ex) Features in PS & CF Baryonic oscillation in PS Baryonic bump in CF of deep redshift sample  Ωm, ΩΛ, w We know actual length! Acoustic oscillation : amplitude depends on Ωb scale = comoving sound horizon ‘s’ at last scattering kA = 2π/s depends strongly on Ωm, weakly on Ωb not on DE  Curvature of space, Baryonic mass

SDSS DR5 Best fit m=0.26 (Percival et al. 2007) Main galaxies and LRGs BAO+HST h=0.72 BAO+WMAP3 Best fit m=0.26

Power Spectrum from CMB & LSS : Ωm But biasing relative to matter

Linear scale structures do not change shape (Springel) Linear scale structures do not change shape Intrinsic topology of LSS insensitive to biasing & redshift distortion

LSS topology as a standard ruler Primordial density Dark matter at z=0 LSS topology as a standard ruler Dark halos at z=0 in r Dark halos at z=0 in z 25h-1Mpc Gaussian smoothing

Cosmological parameter estimation from LSS topology curvature in P(k) => genus(λ) depends on cosmology Inconsistency test ! given z => choose a cosmology, i.e. r(z) => measure genus(λ) => compare model prediction & measurement of genus

Constraint on Ωm better than WMAP3

Properties of non-linear structures

? LSS CMBR 70s BB+(γ,ν; baryon)+GI Dark matter 82Inflation 80s CMBR dT/T < 10-4 Late70s Discovery of LSS mid80 SCDM Model BB+Inflation+(γ,ν; baryon, CDM)+GI 92 COBE dT/T~10-5 92 LSS P(k) SCDM Model ruled out 98 Accelerating expansion 00-03 WMAP Cℓ >2000 Concordance LCDM Model BB+Inflation+(γ,ν; baryon, CDM; Dark E)+GI SDSS JWST many more Planck ? Topology of space; matter contents; matter fluctuation & structure formation

Small scale 1/√N reduction Decoupling surface Acoustic oscillation Small scale 1/√N reduction & Photon diffusion Width Δz=195 Δr=44Mpc 1. Inflation  Same initial phase of oscillation  peaks & troughs in PS 2. Baryonic λJb 2200Mpc ≫ Horizon rHdec 320Mpc > Sound horizon λs 270Mpc > Width Δr 44Mpc > Photon Diffusion λD 14Mpc

3. Gaussianity of ΔT/T Minkowski functionals G(ν)=(Nhot-Ncold)/2πA  Gaussian: No frequency, scale dependence ! Non-Gaussianity Detected! (Park & Park 03)