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

Mass and Light of A1703, A370 & RXJ1347-11
1.5
0.25
Distortion g +
0.2
0.15
0.1
0.05
0
−0.05 0.2
Fraction 1−g +
(G)/g +
(B)
1
0.5
0
g x
0
−0.2
1 2 5 10 20
θ [arcmin]
−0.5
1 2 5 10 20
θ [arcmin]
0.8
1.5
0.7
0.6
Distortion g +
0.5
0.4
0.3
0.2
0.1
0
0.2
Fraction 1−g +
(G)/g +
(B)
1
0.5
0
g x
0
−0.2
1 2 5 10 20
θ [arcmin]
−0.5
1 2 5 10 20
θ [arcmin]
1.5
0.5
Distortion g +
0.4
0.3
0.2
0.1
0
−0.1 0.2
Fraction 1−g +
(G)/g +
(B)
1
0.5
0
g x
0
−0.2
1 2 5 10 20
θ [arcmin]
−0.5
1 2 5 10 20
θ [arcmin]
Figure 3.6 – Tangential reduced shear vs.
radius for A1703, A370 and RXJ1347-11
(top to bottom). The lower panels show the
45 ◦ -rotated (g X ) component of the reduced
shear. The green pentagrams represent the
green sample, containing mostly cluster and
some background galaxies whose colors are
similar to the cluster. The black squares
show the level of tangential distortion of the
combined red+blue (triangles and circles,
respectively) samples of the background.
The green pentagrams slightly rise to the
background level at large radii, indicating
the green sample still contains some level of
background galaxies at the outskirts of the
cluster, and is consistent with zero towards
the cluster center where cluster members
dominate the green sample and dilute the
lensing signal.
Figure 3.7 – Fraction of cluster membership
vs. radius for A1703, A370 and
RXJ1347-11 (top to bottom). Cluster
membership is proportional to the dilution
of the distortion signal of the green sample,
relative to the expected distortion of the
background galaxies set by the combined
red and blue samples. The fraction departs
from unity only at large radius.