Weak lensing by large scale structure

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What does the signal mean? non-linear physics The matter power spectrum (analogous to the that of the CMB) is one way to represent the measurements.
What does the signal mean? The cosmic shear signal is mainly a measurement of the variance in the density fluctuations. Same “lensing” signal Little bit of matter, large fluctuations Lot of matter, small fluctuations To first order lensing measures a combination of the amount of matter Ω m and the normalisation of the power spectrum σ 8.
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: Simulations So far two papers have
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 and 48: CFHTLS: recent results Cosmology is
Page 49 and 50: CFHTLS: what is next? Currently ~14
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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