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

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Introduction stellar-scale lensing are unlikely to be resolved, Zwicky (1937) argued that multiple images due to lensing by galaxies will lie at large enough angles to be observed and would serve as another measure of galaxy masses. Such an independent method was needed in order to test the emerging evidence that galaxies weigh about two orders of magnitude more than their stellar content. The first example of multiple images due to gravitational lensing was discovered when a double-imaged quasar was measured by Walsh, Carswell, & Weymann (1979). The two images of QSO 0957+561 were shown to be of the same quasar being lensed by a foreground galaxy. This discovery transformed gravitational lensing from a theoretical idea to a valid experimental field with cosmological applications. More examples of lensing soon followed. In the massive Abell 370 cluster, a peculiar “ring-like” shape was discovered by Soucail et al. (1987a) and independently by Lynds & Petrosian (1986), thought at first to be the result of galaxy/galaxy interactions in the cluster itself. It was only later recognized to be a strong lensing “giant arc”, occurring when the source is lying behind the lens close to a caustic (Soucail et al. 1987b; Paczynski 1987). Apart from these spectacular examples of strong lensing which are quite rare and are only seen in the center, clusters overall coherently distort (and amplify) fainter background galaxies on a weaker scale, referred to as “weak lensing” (Fort et al. 1988). Using these observations to reconstruct in a model-independent way the two-dimensional mass map of the cluster was suggested by Kaiser & Squires (1993) and has been subsequently measured for many clusters (Bonnet et al. 1993; Smail & Dickinson 1995; Broadhurst et al. 1995). In the past decade major improvements have been made in the field of weak lensing, due to the development of algorithms that robustly measures accurate galaxy shapes by overcoming inherent systematics (Kaiser et al. 1995), and on the other level the recent construction of large telescopes with wide-field cameras that enable imaging of clusters to their virial radius with increasingly higher resolution. This set the ground for numerous cluster mass reconstruction studies both in the strong (Kneib et al. 1996; Hammer et al. 1997; Sand et al. 2002; Gavazzi et al. 2003; Sand et al. 2004; Broadhurst et al. 2005a; Sharon et al. 2005) and weak lensing regimes (Kneib et al. 2003; 12
1.2 Gravitational Lensing Broadhurst et al. 2005b; Limousin et al. 2007; Jee et al. 2009). The cosmic shear technique is based on measuring the distortions to galaxies induced by the Large Scale Structure (LSS). Formalisms that crosscorrelate the foreground structures along the line of sight with the distribution of background images were developed (Wittman et al. 2001; Jain & Taylor 2003; Bacon et al. 2003; Taylor et al. 2007). Cosmic shear was recently statistically detected in large random patches of the sky including the COMBO-17 fields (Brown et al. 2003; Kitching et al. 2007) and the COSMOS field (Massey et al. 2007). These cosmic shear surveys provide a direct measurement of the LSS, and can be compared to theories of structure formation, thereby opening wide prospects for studying cosmology. To usefully derive cosmological parameters from general cosmic shear work, deep all-sky surveys have been proposed (e.g., LSST 1 , DES 2 , JDEM 3 , EUCLID 4 ) and will commence in the coming decade. 1.2.2 Principles of Gravitational Lensing In Figure 1.1 a typical case of gravitational lensing is portrayed. If a mass at redshift z d deflects light from a source at z s , and its size is much smaller than the angular diameter distances D d (observer to lens) and D ds (lens to source), the deflection can be describes by two straight light rays as in the figure. The angle between the two lines is called the “deflection angle” ˆ⃗α, which depends on the mass. 1.2.2.1 The Deflection Angle In the simple case of deflection by a point mass M, where the light ray travels far enough from the horizon of the lens, i.e., it’s impact parameter is much 1 http://www.lsst.org/lsst 2 https://www.darkenergysurvey.org/ 3 http://jdem.gsfc.nasa.gov 4 http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=42266 13
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Chapter 3 Detailed Cluster Mass and
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3.6 Weak lensing analysis 3.6 Weak
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3.8 Cluster light profiles 600 A168
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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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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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