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

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WL Determination of the Distance-Redshift Relation covering a very wide range of wavelength. Note that with only three bands, only a small fraction of the objects have well defined photometric redshifts, in the sense of having a single, narrow peak in their probability p(z), and therefore their use to separate among different redshift populations is very limited. Using the BRz ′ CC space in this way with reference to the now well established redshift surveys is arguably more reliable in separating galaxy populations of differing depths, in agreement with the simulations of Jain et al. (2007). In our previous analysis of this cluster, (Medezinski et al. 2010, hereafter M10), we demonstrated how the cluster and foreground galaxies can be reliably identified and separated from background galaxies in the CC diagram, using B J , R C , z ′ bands (Fig. 4.1). We found in the field of A370 the prominent overdensity of galaxies centered on B J − R C ∼ 2 and R C − z ′ ∼ 0.8 denotes the red-sequence of cluster galaxies (see Fig. 4.1, left-hand panel, where this overdensity is enclosed by white dashed line). This was also shown by the relatively small mean distance from cluster center of galaxies in that region in CC space (Fig. 1 in M10). The WL measurements for this population of objects is very close to zero, with a measured tangential distortion profile, g T (r), consistent with zero all the way out to the virial radius, as expected for cluster galaxies which are unlensed. The main central overdensity around B J − R C ∼ 1 and R C − z ′ ∼ 0.3 consists of many foreground galaxies (see Fig. 4.1, left-hand panel, with an overdensity enclosed by solid white line). These galaxies show a very low level g T compared to the reference background, marked in gray on Fig. 4.1 (right panel), and their surface density profile shows only modest central clustering (see M10) indicating that most of these objects lie in the foreground of the cluster. We use a bright subsample of these foreground galaxies to demonstrate the zero-level signal at a redshift point below the cluster (see below § 4.5), marked in gray on Fig. 4.1 (bottom panel). When selecting background galaxies we stay well away from these regions to minimize contamination by these unlensed galaxies, as described below. To identify background populations in M10, we took into account both 118
4.3 Sample selection from the color-color diagram the WL signal and the density distribution of galaxies in the CC plane. In CC space a relatively red population can be rather well defined, dominated by an obvious overdensity (around B J − R C ∼ 0.5 and R C − z ′ ∼ 0.8), and the bluest population is confined to a separate cloud (around B J − R C ∼ 0.3 and R C − z ′ ∼ 0.2) of faint galaxies with a clear lensing signal. Looking at the WL profiles of the red and blue samples, we see very similar behavior, with a continuous rising signal toward the cluster center. Both cases show good agreement with each other (M10). Combined together, they form our reference background sample, to which all the other samples we derive below will be normalized. The validity of our selection was also demonstrated in M10 by comparison with the spectral evolution of galaxies calculated with the stellar synthesis code Galev 6 (Kotulla et al. 2009). Here we overlay the CC diagram with color-tracks of galaxy models: E-type (exponentially declining SFR with Z ⊙ ), S0 (gas-related SFR with Z ⊙ ), Sa (gas-related SFR with 2.5Z ⊙ ), and Sd (constant SFR with 0.2Z ⊙ ). These evolutionary tracks originate in the low-redshift cloud we established as foreground in CC space and evolve to higher redshift passing through the cluster redshift and then to bluer colors as shown in Fig. 4.5 (right), and finally end at the top-left corner of our CC space, dropping out of the B J -band at a redshift of z ∼ 3.5 In this paper we add additional samples of background galaxies. Two samples will consist of galaxies at redshifts not far beyond that of the cluster, which we term “orange” and “green”. These are selected to lie on the upper-right of the CC space, corresponding reasonably to color-tracks of E/S0 galaxies which are predicted to show a bend in the CC plane, becoming bluer (B J − R C ∼ 2 − 2.5 and R C − z ′ ∼ 1 − 1.5) toward higher redshift, matching well our observed distribution. A third group comprises the red-cloud described above, centered on B J − R C ∼ 0.5 and R C − z ′ ∼ 0.8, we call the “red” sample. This sample consists of an overdensity of background galaxies from the known “red” branch of the bimodality of field galaxies colors (Capak et al. 2007). A Forth sample consists of the prominent blue peak 6 http://www.galev.org/ 119
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Chapter 1 Introduction Clusters of
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Page 163 and 164: REFERENCES Broadhurst, T., Umetsu,
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