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

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Weak Lensing Dilution in A1689 30 28 Radial critical curve κ=1 curve 26 24 θ [arcsec] 22 20 18 16 14 12 0 5 10 15 20 25 30 C Vir Figure 2.20 – The curves shows how the radius of the radial critical curve, shown in blue, varies with the concentration parameter of an NFW profile, where the model is normalized to generate the observed Einstein radius of 47 ′′ for all values of the concentration parameter, C vir . The radial critical curve shrinks as the mass profile becomes steeper. This is also the case for the radius at which the distortion g T = 0, corresponding to the radius where the surface density of matter is equal to the critical surface density (κ = 1), here the degree of tangential and radial distortion is always equal, independent of the form of the mass profile. We have marked the observed values of the radial critical curves and the radius where the distortion is seen to be zero as measured independently in two ways using the statistical distortion measurements (dotted lines) as described in § 2.4, and the same values derived from the multiple image analysis presented in Broadhurst et al. (2005a) (dashed lines). These differing measurements are consistent with each other and by comparison with the model curves bracket intermediate values of concentration in the range 5 < C vir < 15 for the inner strongly lensed region.
2.B Non-linear effect in the reduced shear estimate 10 0 θ [arcmin] c vir =27 c vir =14 c vir =8 c vir =5 Distortion g + 10 −1 10 −2 0 2 4 6 8 10 12 14 16 Figure 2.21 – NFW models are compared with the measured values of g T for the red+blue background sample described in § 2.2. The models are normalized to match the observed Einstein radius of 47 ′′ . A relatively high concentration is preferred with the best fit corresponding to C vir = 27 −5.7 +3.5 (black curve), for the bulk of data, r > 1.5′ , excluding the strong region where the measured distortions required a significant correction for the finite source sizes. The anticipated low concentration of C ∼ 5 (pink curve) is obviously excluded by the data. For reference we also overplot the purely isothermal profile normalized to the observed Einstein radius (red dotted curve). It also overpredicts the data.
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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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1.2 Gravitational Lensing increase
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1.2 Gravitational Lensing Broadhurs
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1.2 Gravitational Lensing If we ins
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1.2 Gravitational Lensing Figure 1.
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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 1.6 1.4 1.2 Γ (g T amp
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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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