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

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Mass and Light of A1703, A370 & RXJ1347-11 with other observables in a more statistically robust way. Our previous work demonstrated the importance of carefully selecting a background population to avoid contamination by the lensing cluster. It is not sufficient to simply exclude a narrow band containing the obvious E/S0 sequence, following common practice, because the lensing signal of the remainder bluer objects is found to fall rapidly towards the cluster center relative to the background of red lensed galaxies indicating that unlensed cluster members are present blueward of the sequence diluting the true lensing signal (Broadhurst et al. 2005b). Due to this effect, many WL studies have underestimated the masses and concentrations of cluster mass profiles (Lu et al. 2009), a point now widely acknowledged (Limousin et al. 2007; Oguri et al. 2009; Okabe et al. 2009). This effect resolved the long standing discrepancy between the strong and WL effects, with the WL signal underpredicting the observed Einstein radius by a factor of ∼ 2.5 (Clowe & Schneider 2001; Bardeau et al. 2005), based only on a minimal rejection of obvious cluster members using one or two-band photometry. Red background galaxies behind clusters have since been explored carefully with deep wide-field spectroscopy by Rines & Geller (2008), who emphasize that the red population in their cluster data comprises exclusively background objects. This lensing “dilution” effect may be turned to our advantage as a means of correcting the cluster population for background contamination, extending the work of Medezinski et al. (2007). Here we analyze very high quality Subaru images of A1703, A370, & RXJ1347-11 for which we have accurate WL measurements. For these clusters, a wider range of colors is available than for A1689, which we make full use here to improve the separation of cluster members from foreground and background populations using the color-color (CC) diagram and application of our dilution method. Using the dilution method has the advantage that it does not require the actual subtraction of background galaxies which introduces the inherent uncertainty caused by the clustering of the background signal and the attendant requirement for the accurate photometry of control fields. In § 3.2 we present the cluster observations, the data reduction, and in 78
3.2 Subaru data reduction § 3.3 we explain how we select cluster galaxies, background samples, and foreground samples. In § 3.4 we examine evolutionary tracks to reinforce the sample selection criteria, and compare with blank-field surveys to determine redshift distributions in § 3.5. In § 3.6 we describe the WL analysis, and in § 3.7 we describe how the WL measurements are used to determine the cluster fraction using our WL dilution method. In § 3.8 we derive the light profile of each cluster, and compare with the mass profile to obtain the M/L profile in § 3.9. In § 3.10 we investigate the shape and variation of the cluster luminosity functions (LF) and its radial dependence. Finally, we summarize our findings in § 3.11. The ΛCDM cosmological model is adopted, with Ω M = 0.3, and Ω Λ = 0.7, but with h left in units of H 0 /100 km s −1 Mpc −1 , for easier comparison with earlier work. 3.2 Subaru data reduction We analyze deep images of three intermediate-redshift clusters, A1703 (z = 0.258), A370 (z = 0.375) and RXJ1347-11 (z = 0.451), observed with the wide-field camera Suprime-Cam (Miyazaki et al. 2002) in several optical bands, at the prime focus of the 8.3m Subaru telescope. The cluster A1703 was observed on 2007 June 15 and the WL signal analyzed by Broadhurst et al. (2008) and Oguri et al. (2009). The observations of the other two clusters are available in the Subaru archive, SMOKA 1 . Subaru reduction software (SDFRED; Yagi et al. 2002; Ouchi et al. 2004) is used for flat-fielding, instrumental distortion correction, differential refraction, sky subtraction, and stacking. Photometric catalogs are created using SExtractor (Bertin & Arnouts 1996) in dual-image mode, for which we use our deepest band as the detection image. Since our work relies heavily on the colors of galaxies, we prefer using isophotal magnitudes. Astrometric correction is done with the scamp tool (Bertin 2006) using reference objects in the NOMAD catalog 1 http://smoka.nao.ac.jp. 79
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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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Chapter 1 Introduction Clusters of
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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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