Weak lensing by large scale structure

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CFHTLS: recent results Results agree well with WMAP3 (and WMAP5…)
CFHTLS: what is next? Currently ~140 sq. deg. of data have the full ugriz coverage and photometric redshift have been determined. With photometric redshift information for the sources we can study the growth of <strong>structure</strong>, which significantly improves the sensitivity to cosmological parameters.
Page 1 and 2: We ak Lens ing by Large-scale Struc
Page 3 and 4: How to proceed? We have a number of
Page 5 and 6: Look at the bright side? We can sim
Page 7 and 8: Simulating the Universe GIF simulat
Page 9 and 10: Gravitational lensing As predicted
Page 11 and 12: Gravitational lensing
Page 13 and 14: Gravitational lensing Strong gravit
Page 15 and 16: Weak gravitational lensing Credit:
Page 17 and 18: Weak lensing mass calibration Obser
Page 19 and 20: Hoekstra et al. (submitted) Quantif
Page 21 and 22: Cosmic shear is everywhere Credit:
Page 23 and 24: Why cosmic shear? Current observati
Page 25 and 26: What do we need to do? We only need
Page 27 and 28: What do we need to do? The weak len
Page 29 and 30: ... put it on a good telescope ...
Page 31 and 32: Systematics The observational disto
Page 33 and 34: E-mode (curl-free) B-mode (curl) Di
Page 35 and 36: Simulations So far two papers have
Page 37 and 38: What does the signal mean? The cosm
Page 39 and 40: Results: a decade ago... This page
Page 41 and 42: Results: status in 2003 CMB Lensing
Page 43 and 44: CFHTLS: first results ~20 square de
Page 45 and 46: CFHTLS: first results Since the pub
Page 47: CFHTLS: recent results Cosmology is
Page 51 and 52: Tomography works! Redshift dependen
Page 53 and 54: Evidence for dark energy From COSMO
Page 55 and 56: Averaged shape: Do we understand? A
Page 57 and 58: Further ahead... The study of dark
Page 59: Conclusions The CFHTLS weak lensing

Weak lensing by large scale structure

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