## Efficiency of weak lensing surveys to probe cosmological models
^{1} CITA, 60 St Georges Str., Toronto, M5S 3H8 Ontario,
Canada^{2} MPA, Karl-Schwarzschild-Strasse 1, Postfach 1523,
D-85740 Garching, Germany^{3} OMP, 14 avenue Edouard Belin, F-31400 Toulouse,
France^{4} Service de Physique Théorique, C.E. de
Saclay, F-91191 Gif-sur-Yvette Cedex, France^{5} Institut d'Astrophysique de Paris, 98 bis, boulevard
Arago, F-75014 Paris, France^{6} Observatoire de Paris, DEMIRM, 61, avenue de
l'Observatoire, F-75014 Paris, France
We apply a mass reconstruction technique to large-scale structure gravitational distortion maps, simulated for different cosmological scenarii on scales from 2.5 arcmin to 10 degrees. The projected mass is reconstructed using a non-parametric least square method involving the reduced shear on which noise due to intrinsic galaxy ellipticities has been added. The distortion of the galaxies is calculated using the full lens equation, without any hypothesis like the weak lensing approximation, or other linearization. It is shown that the noise in the reconstructed maps is perfectly
uncorrelated Poissonian, with no propagation from short to large
scales. The measured power spectrum and first four moments of the
convergence can be corrected accurately for this source of noise. The
cosmic variance of these quantities is then analyzed with respect to
the density of the background galaxies using 60 realizations of each
model. We show that a moderately deep weak lensing survey
( degrees with a typical background
population of gal/arcmin Remarkably, we have found that, using the third moment of the local convergence only, such a survey would lead to a separation between open () and flat () models. This separation does not require a very deep survey, and it is shown to be robust against different hypothesis for the normalization or the shape of the power spectrum. Finally, the observational strategy for an optimal measurement of the power spectrum and the moments of the convergence is discussed.
This article contains no SIMBAD objects. ## Contents- 1. Introduction
- 2. Generation of realistic -maps
- 3. Power spectrum analysis of the reconstructed maps
- 4. Moments in real space
- 4.1. Signature of the normalization and non-Gaussian properties
- 4.2. Top-hat versus compensated filters
- 4.3. Moment estimations and shot noise corrections
- 4.4. Results
- 4.4.1. Noise correction
- 4.4.2. The variance
- 4.4.3. The skewness
- 4.5. Comparisons of different observational scenarios
- 4.5.1. Effect of the survey size
- 4.5.2. Effect of the source redshift
- 4.6. BG versus CDM power spectrum
- 4.7. Effect of the normalization
- 4.8. Beyond the skewness to measure ?
- 5. Discussion
- 6. Conclusion
- Acknowledgements
- Appendix
- References
© European Southern Observatory (ESO) 1999 Online publication: December 22, 1998 |