1. Weak lensing mass-selected cluster catalogues Richard Massey (CalTech) with Jason Rhodes (JPL), Alexie Leauthaud (Marseille), Justin Albert (CalTech), Joel Berg é (Saclay), Richard Ellis (CalTech), Alexis Finogeunov (Garching), Luigi Guzzo (INAF), Catherine Heymans (UBC), Jean- Paul Kneib (Marseille), Alexandre Refregier (Saclay), Nick Scoville (CalTech), James Taylor (CalTech), Ludovic Van Waerbeke (UBC) and the COSMOS team Weak lensing mass maps from the HST COSMOS survey

2. Weak gravitational lensing: patterns in a shear field Clusters are patterns in a shear field:

3. Mass map of COSMOS survey

4. Mass map of COSMOS survey (zoom) Multiscale wavelet reconstruction method of Starck et al. (2005)

5. Mass map of COSMOS survey

6. Residual systematics (“B modes”)

7. Effect of CTE trailing

8. Lensing sensitivity with redshift Number of resolved galaxies z

9. Mass vs light See poster upstairs by James Taylor; light map from Nick Scoville

10. Mass vs light

11. Mass vs x-rays Gunther Hasinger, Alexis Finoguenov & Nico Cappelluti

12. Mass vs x-rays Alexis Finoguenov & James Taylor

13. Zoom to one cluster at z=0.73 Lensing X-ray Guzzo et al. (2006) Cassata poster upstairs

14. Lensing sensitivity function (split)

15. Lensing sensitivity function (tomography) Number of resolved galaxies z

16. Tomography (3D maps), z~0.3 ~19Mpc  19Mpc

17. Tomography (3D maps), z~0.5 ~26Mpc  26Mpc

18. Tomography (3D maps), z~0.7 ~31Mpc  31Mpc

19. PRELIMINARY! Completely 3D maps… Courtesy David Bacon

20. PRELIMINARY! Completely 3D maps… Courtesy David Bacon

21. Conclusions PSCz galaxy density < 150 Mpc/h Reconstructed mass maps provide, for the first time, a direct view of the large-scale, filamentary distribution of dark matter. Optimally-tuned lensing analysis around identified structures links into astrophysics (MD relation, x-ray MT, cluster formation…) COSMOS mass density