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

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Weak Lensing Dilution in A1689 bluer colors. The green galaxy sample is simply selected to lie between the red and blue samples defined above, (V − i ′ +0.1 ) E/S0 (Fig. 2.1), with generous limits −0.3 set to include the vast majority of cluster galaxies, since - as we have established - both the red and blue samples are negligibly contaminated by cluster members, and hence the vast majority of cluster members must lie within this intermediate range of color. A narrow gap on each side of these samples is left out of our analysis to ensure that the definition of the background does not encroach on the cluster population. Note that unlike the green sample containing the cluster population, the background populations do not need to be complete in any sense but should simply be well defined and contain only background. Increasing the green sample to cover these narrow gaps does not lead to any particularly significant change in our conclusions, but only increases somewhat the level of noise by including relatively more background galaxies. Within the green sample there are of course background galaxies, and the purpose of this paper is to make use of the relative proportion of these cluster and background populations via weak lensing to establish the properties of the cluster galaxy population, by using the the dilution of the weak lensing signal of the background galaxies due to the cluster members. 2.3 Distortion analysis of subaru images We use the IMCAT package developed by N. Kaiser 2 to perform object detection, photometry and shape measurements, following the formalism outlined in (Kaiser, Squires, & Broadhurst 1995, hereafter KSB). We have modified the method somewhat following the procedures described in Erben et al. (2001, see Section 5). To obtain an estimate of the reduced shear, g α = γ α /(1 − κ), we measure the image ellipticity e α from the weighted quadrupole moments of the surface brightness of individual galaxies. Firstly the PSF anisotropy needs to be 2 http://www.ifa.hawaii/kaiser/IMCAT 34
2.3 Distortion analysis of subaru images 0.14 0.12 0.1 0.08 0.06 0.04 0.02 0 −0.8 −0.6 −0.4 −0.2 0 0.2 0.4 0.6 color−(red sequence) Figure 2.2 – To establish the boundaries of the color distribution free of cluster members we calculate the mean tangential distortion averaged over the full radial extent of the cluster, done separately for the blue and red samples. On the right the red curve shows that g T drops rapidly when the bluer limit of the entire red sample is decreased below a color while lies +0.2 mag redward of the cluster sequence. This sharp decline marks the point at which the red sample encroaches on the E/S0 sequence of the cluster. On the blue side the red limit of the blue sample is chosen to lie −0.45 mag blueward of the cluster sequence, marking the point at which significant contamination by the cluster acts to dilute the weak lensing signal from later-type bluer cluster members. corrected using the star images as references: e ′ α = e α − P αβ smq ∗ β (2.1) where P sm is the smear polarizability tensor being close to diagonal, and qα ∗ = (P ∗sm ) −1 αβ eβ ∗ is the stellar anisotropy kernel. We select bright, unsaturated foreground stars identified in a branch of the half-light radius (r h ) vs. magnitude (i ′ ) diagram (20 in a smooth map of q ∗ α which is used in equation (2.1), we divided the 9K × 7.4K image into 5 × 4 chunks each with 1.8K × 1.85K pixels, and then fitted the q ∗ in each chunk independently with second-order bi-polynomials, q α ∗ ( ⃗ θ), in conjunction with iterative σ-clipping rejection on each component of the residual e ∗ α − P αβ ∗smq ∗ β (⃗ θ). The final stellar sample consists of 540 stars, or the mean surface number density of n ∗ = 0.72 arcmin −2 . From the rest of the object catalog, we select objects with 2.4 r h 15 pixels as an i ′ -selected weak lensing galaxy sample, which contains 61, 115 35
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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 very moderate decl
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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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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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