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

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Introduction ing of the image, thus diluting or even erasing the real lensing signal. Since galaxies have angular sizes below 1 ′′ , the required seeing for observations should also be below 1 ′′ . Such a limit is not commonly met in many observational sites. The anisotropy in the PSF induced by the telescope optics results in systematic image ellipticities. The PSF has an effect of 8 − 10%, whereas the weak lensing signal is comparable or less (only about 1 − 3% for cosmic shear). It is therefore crucial to model and remove the systematic effects of the PSF with high accuracy. Given that PSF varies significantly with different telescope/CCD configurations and atmospheric situation, this is not a simple task. A number of lensing methods are now able to model this quite well, e.g., the Kaiser, Squires, & Broadhurst (1995) method described above (1.2.3.2), generally using stars along the field to sample the PSF, with robust algorithms for modeling and deconvolving the effect (Heymans et al. 2006; Massey et al. 2007a, for a recent review and comparison of all methods). 1.2.4.2.4 Weak Lensing Dilution It is crucial in cluster weak lensing analysis to carefully select background galaxies in order to avoid contamination by the lensing cluster and/or foreground galaxies. The inclusion of such unlensed galaxies reduces the lensing signal, particularly at smaller distances from the cluster center, where the cluster is relatively dense. When excluding only a narrow band containing the obvious E/S0 sequence, following common practice, the lensing signal of the remainder is found to fall rapidly towards the cluster center, in contrast to the uncontaminated population of background galaxies lying redward of the cluster sequence (Broadhurst et al. 2005b). Other calibration issues in the cluster mass measurement arise from the redshift distribution of the background population which has to be taken into account. In the work presented here I elaborate on and attempt to correct for both these effects. 24
1.3 The Structure of the Thesis 1.3 The Structure of the Thesis The thesis consists of two main scientific efforts: A detailed study of several clusters of galaxies with weak gravitational lensing, and an initial attempt to make cosmological deductions from the study. On one level, I developed new procedures to maximize and improve the way weak lensing is measured in clusters, focusing on a careful selection of galaxies for weak lensing analysis, while benefiting from the “dilution” to learn about the cluster light properties. This work is presented in Chapter 2 for the first cluster examined, Abell 1689. This work was extended to three more high-mass clusters, as described in Chapter 3. On the other level, I examined the distance-redshift relation from the weak lensing of selected samples of background galaxies behind one of the explored clusters, A370, and led the way to a new cosmological probe based on this detectable behavior, as discussed in Chapter 4. 25
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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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3.3 Sample selection from the color
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3.4 Evolutionary color tracks 0.25
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3.5 Depth estimation from SDF/COSMO
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3.6 Weak lensing analysis 3.6 Weak
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3.6 Weak lensing analysis where θ
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3.8 Cluster light profiles 600 A168
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3.9 M/L profiles Broadhurst et al.
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3.9 M/L profiles very moderate decl
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3.11 Discussion and conclusions law
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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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4.5 Results tion N i (z s ) of i-th
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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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