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

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Weak Lensing Dilution in A1689 Using this mass, a bend-angle of α = 4GM(
2.10 Cluster mass profile tangential critical radius of 47 ′′ to match the mean critical radius derived from the data (Broadhurst et al. 2005a). To normalize the models we choose to reproduce the observed Einstein radius of 47 ′′ and compare the predicted location of the radial critical curve and the κ = 1 curve. Figure 2.20 shows that both these radii decrease slowly as the concentration parameter is increased. We have marked the observed values of these radii as determined by two independent observational means. We can use the statistical distortion measurements as described in § 2.4, and the same values derived from the multiple image analysis presented in Broadhurst et al. (2005a). These differing estimates are closely consistent with each other, and by comparison with the model curves bracket intermediate values of concentration in the range 5 < C vir < 15 (Fig. 2.20), a range consistent with the results from a detailed fit to the inner profile measured in Broadhurst et al. (2005a). This is found to be very similar to the independently derived central profile of A1689 from Diego et al. (2005); Zekser et al. (2006); Halkola et al. (2006) Outside the tangential critical radius, for r > 1.5, the distortion measurements are small enough not to suffer from any significant underestimation due to the finite source sizes and we may compare the observed distortion profile, g T (r), out to the limit of our data, r < 15 ′′ . We find this distortion profile is reasonably well fitted by an NFW profile particularly at large radius, 4.0 ′′ < r < 15 ′′ , but with a relatively large concentration, C vir = 27.2 +3.5 −5.7, as shown in Figure 2.21. Note that we have used here a linear radial binning when measuring the concentration parameter and therefore the result here is more weighted by large radius signal than for the analysis of Broadhurst et al. (2005b) where we used logarithmic binning, yielding a smaller value of C vir . This difference in the derived value of C vir is not because of any revision in our estimates of the distortion, in fact both analyses yield very consistent distortion profiles at large radius, but rather that the form of the NFW profile is not consistent with our data over the full radial range - the best fitting NFW model is either too shallow at large radius or too steep at small radius depending where one prefers to fit the data. 63
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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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1.1 Clusters of Galaxies and a grav
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1.1 Clusters of Galaxies to the sph
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1.1 Clusters of Galaxies 1.1.5 X-ra
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Chapter 4 A Weak Lensing Determinat
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4.1 Introduction Zitrin et al. 2009
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4.3 Sample selection from the color
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4.4 Weak lensing measurements objec
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4.5 Results tion N i (z s ) of i-th
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4.5 Results n [arcmin −2 ] 10 1 1
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4.5 Results 3.5 3 2.5 4 3.5 3 B −
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4.5 Results 0.4 0.35 0.3 0.25 foreg
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4.5 Results Γ (g T amplitude ratio
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4.5 Results 1.6 1.4 1.2 Γ (g T amp
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4.7 Discussion and conclusions is t
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Chapter 5 Discussion 5.1 Summary In
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5.1 Summary excluding the foregroun
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5.3 Future work observations we obt
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References Abadi, M. G., Moore, B.,
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REFERENCES Broadhurst, T., Umetsu,
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REFERENCES Gaidos, E. J. 1997, AJ,
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REFERENCES Kaiser, N. 1995, ApJ, 43
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REFERENCES Natarajan, P., Loeb, A.,
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REFERENCES Schrabback, T. et al. 20
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כפי שמתואר בפרק השל
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עבודה זו נעשתה בהנח
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