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

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WL Determination of the Distance-Redshift Relation for blue galaxies, or even simply a limiting magnitude beyond which the photo-z method fails in this catalog. We set our magnitude limits conservatively to minimize these possible problems, with 19 < z ′ < 23 for the orange sample, 20 < z ′ < 24.5 for the green sample, 23 < z ′ < 25 for the blue sample, 22 < z ′ < 26 for the red sample, and 24.5 < z ′ < 26.5 for the dropout sample. 4.5.4 Lensing strength vs. redshift We may now finally combine the WL distortion information with the redshift information for all the samples of background galaxies defined above. In order to compare the resulting trend with the cosmological trend, we plot Γ, the g T -amplitude ratio, against median redshift, 〈z s 〉, in Fig. 4.9. Each point in the figure represents an independent sample, where the first point represents the foreground sample in front of the cluster, and the other points represent background galaxy samples. For each sample, we also calculate the median lensing distance ratio, 〈D ds /D s 〉, for each cosmological model – ΛCDM (empty circles), Einstein-de Sitter (crosses), and an empty universe (empty squares), using the COSMOS photo-z measurements of galaxies within the same CC-magnitude boundaries defined for each background sample and thus obtain the predicted depth. We interpolate between these discrete predicted values to provide the theoretical relation, D ds /D s (z) for each cosmological model. We can thus compare how the WL strength Γ agrees with predicted D ds /D s . A clear trend of increasing WL amplitude is seen with redshift. A null result of no distance-redshift increase is easily excluded with low significance – χ 2 /N = 91/8. It is evident that the WL amplitude agrees well with the theoretical relations for D ds /D s as a function of redshift, rising steeply behind the lens and saturating at high redshifts, albeit currently consistent with a wide range of cosmologies. 134
4.5 Results 1.6 1.4 1.2 Γ (g T amplitude ratio) 1 0.8 0.6 0.4 0.2 0 ΛCDM; χ 2 /N=3.4/8 EdS; χ 2 /N=3.3/8 Ω M =0,Ω Λ =0; χ 2 /N=3.5/8 −0.2 0 0.5 1 1.5 2 2.5 3 3.5 4 Figure 4.9 – g T amplitude ratio, Γ, vs. redshift for A370 bright (stars) and faint (circles) samples. Also plotted is the lensing depth, D ds /D s , vs. redshift for different cosmologies - ΛCDM (circles+solid line), Einstein-de Sitter (crosses+dashed line), and an empty Universe (squares+dashed-dotted line) estimated using the COSMOS photometric redshift catalog.
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TELAVIVUNIVERSITY SCHOOLOFPHYSICS&A
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To my parents
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1.2.3 Weak Gravitational Lensing .
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5 Discussion 139 5.1 Summary . . .
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negligibly contaminated by the clus
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Acknowledgments I would like to tha
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Chapter 1 Introduction Clusters of
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1.1 Clusters of Galaxies The space
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Chapter 3 Detailed Cluster Mass and
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3.1 Introduction Stars are not expe
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Page 167 and 168: REFERENCES Kaiser, N. 1995, ApJ, 43
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