Mass and Light distributions in Clusters of Galaxies - Henry A ...

WL Determination of the Distance-Redshift Relation
g T
g T
g T
g T
g T
1
0.5
0
1
0.5
0
1
0.5
0
1
0.5
0
1
0.5
0
θ [arcmin]
θ [arcmin]
θ [arcmin]
θ [arcmin]
1 2 5 10
θ [arcmin]
χ 2 Γ=−0.04±0.1
/dof = 13/6
χ 2 Γ=0.41±0.2
/dof = 1/6
χ 2 Γ=0.85±0.2
/dof = 11/6
χ 2 Γ=0.87±0.1
/dof = 17/8
χ 2 Γ=0.95±0.2
/dof = 6/8
g T
g T
g T
g T
1
0.5
0
1
0.5
0
1
0.5
0
1
0.5
0
θ [arcmin]
θ [arcmin]
θ [arcmin]
1 2 5 10
θ [arcmin]
χ 2 Γ=0.88±0.2
/dof = 6/7
χ 2 Γ=1±0.1
/dof = 27/8
χ 2 Γ=1.1±0.2
/dof = 23/8
χ 2 Γ=1.3±0.2
/dof = 13/8
Figure 4.4 – g T vs. cluster radius for A370 bright samples (top: foreground, orange,
green, red & blue) and faint (bottom: green, red, blue & dropouts), where the fixed
power-law fit is overlaid (dashed black line) with 1 − σ confidence levels (shaded region).
Also plotted is the power-law fit of the equivalent “reference” background sample (dotted
curve). In each case the resulting normalized g T amplitude ratio, Γ, is denoted next to
the profile.