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

3.11 Discussion and conclusions
Table 3.3 – Parameters of Schechter fits to the Luminosity function
Cluster radial range α M ∗
(h −1 Mpc)
A1703 0 − 0.3 −0.95 ± 0.05 −21.4 ± 0.6
0.3 − 0.8 −1.08 ± 0.08 −21.7 ± 0.8
0.8 − 2.5 −1.24 ± 0.2 −21.8 ± 3
A370 0 − 0.3 −1 ± 0.04 −22.4 ± 0.6
0.3 − 1 −1.12 ± 0.05 −22.1 ± 0.7
1 − 2.2 −1.18 ± 0.09 −22.8 ± 1
RXJ1347-11 0 − 0.8 −1 ± 0.06 −21.6 ± 0.5
0.8 − 2 −1.12 ± 0.1 −22 ± 2
3.11 Discussion and conclusions
In this paper we have compared in detail the dark and luminous properties of
three high mass galaxy clusters, A1703, A370 and RXJ1347-11, and examined
the relation between mass and light all the way out to the virial radius.
We have further applied the WL dilution approach previously developed for
A1689 (Medezinski et al. 2007) as an alternative means of obtaining the
LF and light profiles of galaxy clusters. This is based on the dilution of the
lensing distortion signal by unlensed cluster members, and has the advantage
of being independent of density fluctuations in the background.
We have examined clusters A1703, A370 and RXJ1347-11 for which data
of exceptional quality has been taken with Subaru/Suprime-Cam in multiple
passbands. We have shown how a careful separation of the cluster,
foreground, and background galaxies can be achieved using weak lensing information
and galaxy colors. We also make use of the clustering of cluster
members, finding the cluster members are confined to a distinct region of
CC space with relatively small mean radial distances. We have constructed
a reliable background sample for WL measurements, by selecting red background
galaxies whose WL signal rises all the way to the center of the cluster,
and adding to those the faint cloud of very blue galaxies, whose WL signal
we have shown is in good agreement with the red galaxies. We have avoided
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