z - KICP Workshops - University of Chicago

1.5
What can we probe?
• Probe Ω =0.2, dark w=-1.0
M energy through the history of the expansion rate:
H 0 r(z)
H 2 (z)
2
H0 = Ωm (1+ z)3 Ω =0.3, w=-1.0
M
+ ΩDE exp[ 3 ∫ (1+ w(z))dln(1+ z) ] Ω =0.2, w=-1.5
M w=−1/3+
( 1− Ωm − ΩDE ) 1+ z
Ω =0.2, w=-0.5
M
1.0
r(z) = ∫ dz'/H(z')
0.1
0.5 • and the growth of large-scale structure:
0.0
Require both to disentangle Dark Energy from Modified Gravity
Distance vs.
Redshift
0.0
€
0.5 1.0
redshift z
1.5 2.0
• Weak Lensing cosmic shear Distances+growth
• Supernovae Distances
• Baryon Acoustic Oscillations Distances and H(z)
• Cluster counting Distances+growth
• Redshift Distortions Growth
δ(z)/δ(today)
€
1
δρ
( ) 2
ρ (z; Ωm ,ΩDE ,w(z),...)
Growth of
w=−1
10.0
Density
Perturbations
z
1.0
6
0.1