1. SEP.20-21.2006.KIASKIAS WORKSHOP1 Dark Energy Effects on CMB & LSS The 2 nd KIAS Workshop on Cosmology and Structure Formation Seokcheon ( 碩天 large sky) Lee Institute of Physics, Academia Sinica

2. SEP.20-21.2006.KIASKIAS WORKSHOP2 Outline  Observable Impact of DE  BAO, CL, SN, WL  (Im)Perfect Dark Energy Fluid  Effects on CMB and Matter Power Spectrum  Summary

3. SEP.20-21.2006.KIASKIAS WORKSHOP3 Observable Impact of DE  Modification of z–d relation : Baryon Acoustic Oscillations (BAO, R.Kron), SuperNova (SN, G-C Liu), [δD]  Effects on growth of structures : Galaxy CLustering counting (CL, Z.Zheng), Weak Lensing (WL, Sejong Univ), ISW effect (C.G.Park)

4. SEP.20-21.2006.KIASKIAS WORKSHOP4 Observations & Measurements

5. SEP.20-21.2006.KIASKIAS WORKSHOP5 H(z) & δ (z)  Evolution of Background  From WMAP data we can find z eq ~ 5000  Flat Universe is preferred by WMAP. i.e. Ω k = 0  Density fluctuation on small scales (sub-horizon scale)

6. SEP.20-21.2006.KIASKIAS WORKSHOP6 r(z) and dV(z)  FRW metric  Volume element  Proper distance  Comoving coordinate

7. SEP.20-21.2006.KIASKIAS WORKSHOP7 Imperfect DE Fluid  Cosmological fluid  Adiabatic and entropic sound speed (J-C Hwang)  Dark energy rest frame  Anisotropic stress of DE

8. SEP.20-21.2006.KIASKIAS WORKSHOP8 Effects of σ on δ & θ  For large scale source term : -(1+ω)(c_s^2-ω)θ/k^2  ω = -0.8  Dominate metric source term and derive δ to smaller values  k = 1.3 · 10^{-4} Mpc^{-1}  (c_s^2, c_vis^2) = (0,0), (0.6,0),(0,0.6),(0.6,0.6)  δ gets smaller when DE dominate (solid lines)  Θ increases (dashed lines)  ISW id enhanced as c^2 increases

9. SEP.20-21.2006.KIASKIAS WORKSHOP9 ISW Effects  C_{vis}^2 : 1.0, 0.1, 0.01, 0.001, 0  MD : total density grows in order to Φ,Ψ = const.

10. SEP.20-21.2006.KIASKIAS WORKSHOP10 Matter Power Spectrum  C_{vis}^2 = 1.0  Solid line : w=-1.2, c_s^2=1.0 Dash-dotted : w=-0.8,c_s^2=0 Dashed : w=-1.2 c_s^2=0 Thick : w=-0.8, c_s^2=1.0

11. SEP.20-21.2006.KIASKIAS WORKSHOP11 Standard Cosmology  Friedman equations  Critical density and density contrasts  Curvature  Hubble’s law

12. SEP.20-21.2006.KIASKIAS WORKSHOP12 DE vs MG    Quintessence  (Generalised) Chaplygin gas  Tachyon  Mass Varying Neutrino  Modification Of Newtonian Dynamics (MOND)  Cardassian Models  Phantom  f(R) Gravity accelerating universe.

13. SEP.20-21.2006.KIASKIAS WORKSHOP13 Developments of DE program  Stage I : Current Known  Stage II : Anticipation for ongoing projects  Stage III : Comprising currently proposed projects  Stage IV : Comprising Large Survey Telescope (LST) and/or Square Kilometer Array (SKA) and/or Joint Dark Energy Mission (JDEM)

14. SEP.20-21.2006.KIASKIAS WORKSHOP14 Quantifying Progress I  Figure of Merit (FoM) : goodness of a single experiment or a combination of experiments on probing DE.  Choose DE parameterization :  DETF FoM : Reciprocal of Area of the error ellipse in w0-w1 plane that enclose 95% C.L contour.

15. SEP.20-21.2006.KIASKIAS WORKSHOP15 Quantifying Progress II (From DETF Report)

16. SEP.20-21.2006.KIASKIAS WORKSHOP16 BAO  s ~ 150 Mpc : sound horizon at LS  Angular size of BAO, Perpendicular to l.o.s  Radial suppression + photo z : exponential suppression  Spectroscopic survey : H(z)  Eisenstein et.al (05) SDSS LRG correlation function. Observer H =  z/s D A = s / 

17. SEP.20-21.2006.KIASKIAS WORKSHOP17 BAO II  s : sound horizon  Acoustic scale depends o n (  mh2)-0.25  Hu. Sugiyama (96)  (A) Least affected by systematic errors  (A) High z  (D) Least statistical power  Large Synoptic Survey Telescope (UC Davis)

18. SEP.20-21.2006.KIASKIAS WORKSHOP18 CL  Galaxy cluster counting 20,000 clusters to z=1with M > 2 X E14Ms  Spatial clustering of galaxies 300 million galaxies  Compare Observed distribution of clusters to N-body simulations  Mass function shape

19. SEP.20-21.2006.KIASKIAS WORKSHOP19 CL II  differential number of clusters  Differential comoving number density, Jenkins (01), assumption : GC = DM halos  Two point correlation funtion  (A) H(z),  z)  (D) uncertaintities

20. SEP.20-21.2006.KIASKIAS WORKSHOP20 SN  SNAP (SuperNova Acceleration Probe) ~ 2000 SNeIa : 0.1 < z <1.7  CSP (Carnegie Supernova Project) : z < 0.1  SDSS II : 0.1 < z < 0.2  SNLS : 0.8 < z < 1.0  ESSENCE : 0.2 < z < 0.8  (A) most established method  (D) evolution of SNe

21. SEP.20-21.2006.KIASKIAS WORKSHOP21 WL (From T.Tyson)

22. SEP.20-21.2006.KIASKIAS WORKSHOP22 WL II  Planck + 3D WL : 10,000 sq deg to median z = 0.7 (A.Heavens 03)  3D WL accuracy on w 1~3 %  DUNE : 20,000 sq. deg. to z = 0.9 (35 gal/arcmin2) (A. Refreiger)  SNAP : 1,000 sq. deg to z = 1.23 (100 gal/arcmin2)  (A) : greatest potential to constrain w  (D) : limited by systematic errors coming from errors of photo-z (except SKA)

23. SEP.20-21.2006.KIASKIAS WORKSHOP23 Surveys

24. SEP.20-21.2006.KIASKIAS WORKSHOP24 Generalized Gravity Theories I  A broad class of alternative gravity theories (From T.Koivisto)   matter fields  Φ : a scalar field

25. SEP.20-21.2006.KIASKIAS WORKSHOP25 Generalized Gravity Theories II

26. SEP.20-21.2006.KIASKIAS WORKSHOP26 Generalized Gravity Theories III

27. SEP.20-21.2006.KIASKIAS WORKSHOP27 Quintessence Potentials  SL(06)

28. SEP.20-21.2006.KIASKIAS WORKSHOP28 Quartessence (Unification of DM & DE)

29. SEP.20-21.2006.KIASKIAS WORKSHOP29 Quartessence II

30. SEP.20-21.2006.KIASKIAS WORKSHOP30 Summary  As c_{vis}^ 2 ↑, δ↓, θ↑, H/k^2(1+ω)θ↑  As c_{vis}^ 2 ↑, ISW ↑  Effects on MPS occurs only at large scales  CMB’s only sensitive to  Correlation to others BAO, CL, D(g), WL…  Bispectra (? Y. Suto)  DARK ENERGY IS NOWHERE!