Detection of Weak Gravitational Lensing by Large-scale Structure

We report a detection of the coherent distortion of faint galaxies arising from gravitational lensing by foreground structures. This “cosmic shear” is potentially the most direct measure of the mass power spectrum, as it is unaffected by poorly-justified assumptions made concerning the biasing of the distribution. Our detection is based on an initial imaging study of 14 separated 8 × 16 fields observed in good, homogeneous conditions with the prime focus EEV CCD camera of the 4.2m William Herschel Telescope. We detect an rms shear of 1.6% in 8 × 8 cells, with a significance of 3.4σ. We carefully justify this detection by quantifying various systematic effects and carrying out extensive simulations of the recovery of the shear signal from artificial images defined according to measured instrument characteristics. We also verify our detection by computing the cross-correlation between the shear in adjacent cells. Including (gaussian) cosmic variance, we measure the shear variance to be (0.016)± (0.012)± (0.006), where these 1σ errors correspond to statistical and systematic uncertainties, respectively. Our measurements are consistent with the predictions of cluster-normalised CDM models (within 1σ) but a COBE-normalised SCDM model is ruled out at the 3.0σ level. For the currently-favoured ΛCDM model (with Ωm = 0.3), our measurement provides a normalisation of the mass power spectrum of σ8 = 1.5 ± 0.5, fully consistent with that derived from cluster abundances. Our result demonstrates that ground-based telescopes can, with adequate care, be used to constrain the mass power spectrum on various scales. The present results are limited mainly by cosmic variance, which can be overcome in the near future with more observations.