sep.20-21.2006.kiaskias workshop1 dark energy effects on cmb & lss the 2 nd kias workshop on...
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SEP.20-21.2006.KIAS KIAS WORKSHOP 1
Dark Energy Effects on CMB & LSS
The 2nd KIAS Workshop on Cosmology and Structure Formation
Seokcheon ( 碩天 large sky) LeeInstitute of Physics,
Academia Sinica
SEP.20-21.2006.KIAS KIAS WORKSHOP 2
Outline
Observable Impact of DE BAO, CL, SN, WL (Im)Perfect Dark Energy Fluid Effects on CMB and Matter Power Spectrum Summary
SEP.20-21.2006.KIAS KIAS WORKSHOP 3
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)
SEP.20-21.2006.KIAS KIAS WORKSHOP 5
H(z) & δ(z)
Evolution of Background From WMAP data we ca
n find zeq ~ 5000 Flat Universe is preferred
by WMAP. i.e. Ωk = 0
Density fluctuation on small scales (sub-horizon scale)
SEP.20-21.2006.KIAS KIAS WORKSHOP 6
r(z) and dV(z)
FRW metric
Volume element
Proper distance
Comoving coordinate
SEP.20-21.2006.KIAS KIAS WORKSHOP 7
Imperfect DE Fluid
Cosmological fluid Adiabatic and entropic
sound speed (J-C Hwang) Dark energy rest frame Anisotropic stress of DE
SEP.20-21.2006.KIAS KIAS WORKSHOP 8
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 increase
s
SEP.20-21.2006.KIAS KIAS WORKSHOP 9
ISW Effects
C_{vis}^2 : 1.0, 0.1, 0.01, 0.001, 0
MD : total density grows in order to Φ,Ψ = const.
SEP.20-21.2006.KIAS KIAS WORKSHOP 10
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
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