1. Weak lensing mass-selected cluster catalogues Richard Massey (CalTech) with Justin Albert (CalTech), Joel Berge (Saclay), Richard Ellis (CalTech), Takashi Hamana (Tokyo), Jean-Paul Kneib (Marseille), Alexie Leauthaud (Marseille), Satoshi Miyazaki (Subaru), Alexandre Refregier (Saclay), Jason Rhodes (JPL), Nick Scoville (CalTech), James Taylor (CalTech) and the COSMOS team

2. Lensing sensitivity with redshift Number of resolved galaxies z

3. Clusters are just… patterns in a shear field

4. Patterns in a shear field

5. Mass maps from ACS data

6. Residual systematics in ACS data

7. E-mode signal B-mode signal Theory

8. Wavelet reconstruction

9. Mass vs light Nick Scoville

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

11. Tomography (3D maps) Number of resolved galaxies z

12. Tomography (3D maps)

13. Tomography (3D maps): z~0.3

14. Tomography (3D maps): z~0.5

15. Tomography (3D maps): z~0.7

16. Shear measurement from Subaru Deconvolve from the ground-based PSF using shapelets. ~25 galaxies/arcmin 2 with Subaru data, rather than ~60 galaxies/arcmin 2 using ACS Subaru shear (shapelets)

17. Subaru mass maps

19. Residual systematics in Subaru data 1% level residuals

20. FITS versions of all these maps available at: www.astro.caltech.edu/~rjm/mass_mapsConclusions Projected 2D mass maps Somewhat coarser 3D mass maps More optimally-tuned analysis around identified structures Systematics checks: E/B-mode split Systematics checks: ground vs space    