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

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5 Discussion 139 5.1 Summary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 139 5.2 Further application of the methods in other work . . . . . . . 142 5.3 Future work . . . . . . . . . . . . . . . . . . . . . . . . . . . . 143 5.3.1 MCT/CLASH . . . . . . . . . . . . . . . . . . . . . . . 144 References 145 IV
Abstract Clusters of galaxies are the most massive bound objects in the Universe. Their deep potential wells deflect the light of background galaxies creating lensed galactic images. Gravitational lensing can be used as a diagnostic tool to determine the mass profiles of clusters. In the weak lensing regime, the measurement of the cluster mass can be badly compromised by the presence of unlensed foreground and cluster members which dilute the true lensing signal. In this thesis, I study galaxy clusters mass and light properties via weak lensing observations. In the first part, I show the importance of carefully isolating background galaxies from foreground and cluster galaxies for a clean weak lensing measurement, avoiding dilution of the signal. The dilution is in turn used to determine the light properties of the clusters. The second focus of the work shows the use of the detailed measurements to determine the increment of the weak lensing signal with redshift, which is an important cosmological probe. Following an introduction to the field of galaxy clusters and gravitational lensing in Chapter 1, I demonstrate my methods and results for four massive galaxy clusters in Chapters 2 and 3. In Chapter 2 I study cluster A1689 (z = 0.183) with deep Subaru imaging in the V and i ′ bands, using the color-magnitude diagram and the weak lensing signal to derive the luminous properties of cluster galaxies. The tangential distortion of galaxies bluer than the E/S0 sequence falls rapidly toward the cluster center relative to the lensing signal of the background galaxies redder than the sequence. I use this dilution effect to derive the cluster light profile and luminosity function to large radius, with the advantage that no subtraction of far-field background counts is required. The light profile has a constant declining slope , d log(L)/d log(r) = −1.12 ± 0.06 to the limit of the data, r < 2 h −1 Mpc, whereas the mass profile steepens continuously with radius, such that M/L peaks at an intermediate radius, r ∼ 100 h −1 kpc. The cluster luminosity function has a flat faint-end slope, α = −1.05 ± 0.05, independent of radius and with no faint upturn to M i ′ < −12. I show that the bluest objects are V
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2.5 Photometric redshifts Weak Lens
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Weak Lensing Dilution in A1689 30 2
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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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3.2 Subaru data reduction § 3.3 we
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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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3.5 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 10 5 r [Mpc/h] bri
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3.9 M/L profiles very moderate decl
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3.9 M/L profiles 0.6 0.4 0.2 log 10
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3.10 Cluster luminosity functions b
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3.11 Discussion and conclusions Tab
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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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4.4 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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