1. Ludovic Van Waerbeke Department of Physics and Astronomy University of British Columbia Statistical lensing in COSMOS With: F. Bernardeau (CEA) Y. Mellier (IAP) E. Semboloni (IAP) & the COSMOS team

2. Weak lensing two-points statistics: What is measured?  Mass power spectrum normalisation Mass power spectrum normalisation Slope of the power spectrum Slope of the power spectrum Mean density parameter Mean density parameter Redshift of the sources Redshift of the sources ~      z s 1.4  -(n+2)/2 ~      z s 1.4  -(n+2)/2 Contaldi et al. 2004

3. VIRMOS I~24 Z~0.9 LVW et al. COSMOS should reach ~ same accuracy with two major differences: -followups. In particular photoz enables lenses selection, 3D lensing, etc… -morphology -depth enables high order statistics despite small FOV.

4. redshift distributions based on the Hubble deep fields 25.<i<27. Z phot ~1.4

5. Cycle 12 area Polygon masks (ds9 format) are available

6. PSF anisotropy pattern averaged over cycle 12 chips

7. Preliminary E and B modes aperture mass

8. LCDM model with  8 =0.8 and z S ~1.4

9. ~30 stars per chip

10. Needs image reprocessing with smaller pixel size?

11. Star-gal shear aperture correlation

12. Star-gal shear correlation function

13. Strong lensing with R. Gavazzi (OMP, Toulouse)

17. Singular IS Z lens ~0.4 Z source ~3 Re=1.58” M~4.4x10 11 Mo h 70 -1 Inverse pixel mapping into the source plane