Structure Formation and Cosmology with high-z Clusters

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<strong>Clusters</strong> as Gravitational Telescopes
Geometric scaling of Lensing Signal• Geometrically, strong lensing is maximized at low-to-intermediateredshifts, where, for a given mass, #crit is minimalFor a given mass distribution at z=zLz=0.2z=0.5z=0.8zL=0.5zL=0.2zL=0.8zL=1.4zS
Page 1 and 2: Structure Formation and Cosmologywi
Page 3 and 4: Can we extend this work beyond reds
Page 5 and 6: Distribution of baryons and DM in a
Page 7 and 8: Probing the DM mass distribution of
Page 9 and 10: Weak-lensing analysis from HST/ACS
Page 11 and 12: Multiple image system in most dista
Page 13 and 14: Mass components of XMM2235 (at z=1.
Page 15 and 16: The core mass distributionc=3.2c
Page 17: The core mass distributionc
Page 20: WARPSJ1415 at z=1.01 - M200!5"10 14
Page 25 and 26: What makes a cluster an efficient g
Page 27 and 28: Discovery a highly magnified galaxy
Page 29 and 30: Spatial magnification of (strongly)
Page 31 and 32: (1 kpc = 0.2” at z=7.6)likelihood
Page 33 and 34: Typical LBG LBG Candidate Selection
Page 35 and 36: Old HST NIR Camera - NICMOS - 72 or
Page 37 and 38: The advantage of using gravitationa
Page 39 and 40: MACS1149-JD1: z ph= 9.6±0.2Zheng e
Page 41 and 42: The Reionization Epoch with HST27Co
Page 43 and 44: Observational Probes of Cluster For
Page 45 and 46: The colour-magnitude diagram indiff
Page 47 and 48: The Color-Magnitude relation in clu
Page 49 and 50: RDCS1252 (z = 1.24) C-M Relation wi
Page 51 and 52: A Nascent Red Sequence at z&2MRC113
Page 53 and 54: SF histories of ETGs in clusters (a
Page 55 and 56: Measuring metallicity of the ICM at
Page 57 and 58: Out to z=1.4: Chandra Observations
Page 59 and 60: WARPSJ1415 at z=1.01 - M200!5"10 14
Page 61 and 62: Galaxy populations in distant clust
Page 63 and 64: THANKS!XVI IAG/USP Advanced School

Structure Formation and Cosmology with high-z Clusters

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