CMB Angular power spectrum 6000 TT 5000 4000 3000 ±200 00 TE FT 100 500 1000 Multipole moment I ests of perturbation theory
Tests of perturbation theory CMB Angular Power Spectrum
Matter power spectrum Wavelengthλ[h-1Mpc] 104 1000 100 10 10 104 a1000 100 Cosmic Microwave Background ● SDSS galaxies ☆ Cluster abundance 10 a Weak lensing ▲ Lyman Alpha Forest il 0.001 0.01 0.1 10 Wavenumber k [h/Mpc]
Matter Power Spectrum
Dark Energy(DE) Supernova Cosmology Project 3" Big Bang 2 Supernovae q(z=0+z(dg/dz Constant Acceleration. o daldzE 0100 6E 〓〓二 二二二9=一二 749% Dark Energy Coasting, q z) Constant Deceleration.=+.dg/dz:0. 1:01 229 Dark Acceleration+ Deceleration dz=++ Matter 4% Ato
Dark Energy (DE)
H 2 87G Accelerating universe a/ a 4(+3p)>0 Negative pressure W三 <-1/3 Cosmological Constant(Einstein 1917) Rour+ Aguy=-87GTHv v 8G(T+ v 8zg A A A UV(A) dIG v 87G guv=p No perturbation
1/ 3 / ( 3 ) 0 3 4 3 2 8 = − = − + = p w a a p H G G Accelerating universe Negative pressure R Rg g 8G T 2 1 − + = − ) 8 8 ( 2 1 g G R Rg G T − = − + g G T 8 ( ) = = − = g p G 8 w = −1 1, Cosmological Constant (Einstein 1917) No perturbation
Cosmological constant problem Observation P≈(2×10eV 4 Zero point energy density kvk+m M dk 4兀 16丌 M=Mn-10°eV,,~102p
3 4 (2 10 eV) − Cosmological constant problem Observation Zero point energy density + = M v M dk k k m 0 2 4 2 2 2 2 4 16 = 28 121 M Mpl ~10 eV, v ~10