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

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Mass and Light of A1703, A370 & RXJ1347-11 0.35 SDF 0.3 0.25 0.2 P(z) 0.15 0.1 0.05 0 0 0.5 1 1.5 2 2.5 3 3.5 4 z 0.35 COSMOS 0.3 0.25 0.2 N(z) 0.15 0.1 0.05 0 0 0.5 1 1.5 2 2.5 3 3.5 4 z Figure 3.5 – Redshift distributions of CC-selected samples. Two deep field surveys are used to estimate mean redshifts and depth: SDF (top), and COSMOS (bottom). The green (green thin solid line), red (red thick solid line), blue (blue thick dashed line) and foreground (magenta dotted-dashed line) samples are selected according to A370 CC/magnitude limits (see Fig. 3.3).
3.5 Depth estimation from SDF/COSMOS Table 3.2 – CC-selected Sample Properties Cluster Sample magnitude limits N ¯n ¯z s < D ds /D s > arcmin −2 COSMOS SDF COSMOS SDF A1703 green 16.3 < i ′ < 26.5 5678 6.2 0.54 - 0.45 - red 21 < i ′ < 26 4742 5.2 1.00 - 0.67 - blue 22 < i ′ < 26 4467 4.9 1.59 - 0.74 - A370 green 16.5 < z ′ < 26.5 5369 5.3 0.46 0.69 0.25 0.29 red 21 < z ′ < 26 13372 13.7 1.14 1.21 0.57 0.57 blue 22 < z ′ < 26 8481 8.7 1.74 1.65 0.64 0.56 RXJ1347 green 17.5 < z ′ < 26.5 2512 3.5 0.67 0.79 0.28 0.31 red 21 < z ′ < 26 2943 4.1 1.09 1.26 0.49 0.52 blue 22 < z ′ < 26 1691 2.3 1.45 1.67 0.44 0.46 PEGASE templates (Fioc & Rocca-Volmerange 1997) which approximates the library described in Benítez et al. (2004) and Coe et al. (2006). This new library has an accuracy of δz/(1+z) = 0.037 with the FIREWORKS catalog (Wuyts et al. 2009) and a low catastrophic error rate. Using those photo-z, and the spectral classification provided by BPZ, we generate magnitudes in the required Subaru filters to match the cluster observations. We select samples according to CC/magnitude limits described above (Fig. 3.3) for A370 and RXJ1347-11 (the SDF filters are not matched with the filters used for A1703). The resulting redshift distributions of the green (thin solid line), red (thick solid line), blue (dashed line) and foreground (dash-dotted line) samples selected to match A370 samples using SDF are displayed in Fig. 3.5 (top). For COSMOS, photometric redshifts have been derived by Ilbert et al. (2009) using 30 bands in the UV to mid-IR. Since the COSMOS photometry does not cover the Subaru R C band, we need to estimate R C -band magnitudes for it. We use the HyperZ (Bolzonella et al. 2000) template fitting code to obtain the best-fitting spectral template for each galaxy, from which the R C magnitude is derived with the transmission curve of the Subaru R C -band filter (see Umetsu et al. 2010). We then select samples by applying the same CC/magnitude limits as for A1703, A370 and RXJ1347-11. The resulting 91
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To my parents
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1.2.3 Weak Gravitational Lensing .
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negligibly contaminated by the clus
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Chapter 1 Introduction Clusters of
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1.1 Clusters of Galaxies The space
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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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כפי שמתואר בפרק השל
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עבודה זו נעשתה בהנח
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