2. Mapping our Universe for Precision Cosmology Max Tegmark, MIT

3. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 Smorga sbord THE COSMIC SM Ö RG Å SBORD Galaxy surveys Microwave background Gravitational lensing Big Bang nucleosynthesis Supernovae Ia Galaxy clusters Lyman  forest Neutral hydrogen tomography

4. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 What have we learned?

5. Fluctuation generator Fluctuation amplifier Hot Dense Smooth Cool Rarefied Clumpy To 0th order: Cosmological functions   (z), G(z,k), P s (k), P t (k) H(z) (Graphics from Gary Hinshaw/WMAP team) 400 386

6. Fluctuation generator Fluctuation amplifier Hot Dense Smooth Cool Rarefied Clumpy H(z) P(k,z) To 1st order: (Graphics from Gary Hinshaw/WMAP team) 400 386

7. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 Formation movies

8. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 Par movies

9. Cmbgg OmOl 4% 21% 75% Using WMAP + SDSS LRGs:

10. 430 386 13.8

11. Cmbgg OmOl Standard model parameters: Cosmology Particle physics Required Optional C = h = G = k b = q e = 1 

12. What we’ve learned about dark energy from SN Ia Yun Wang, arXiv:0910.2492

13. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 1par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/0207047 + updates CMB

14. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 CMB progress

15. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 exp 9911 CMB Shown at DM2000:

16. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 boom CMB Shown at DM2002:

17. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 105dpi CMB Shown at DM2004:

18. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 Boom zoom For Guth & Kaiser 2005, Science +B03, … Shown at DM2006:

19. Reichardt et al 2008, arXiv:0801.1491 Shown at DM2008:

20. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 WMAP7 2010

21. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 148 GHz J. W. Fowler et al, arXiv:1001.2934

22. But where have all the clusters gone? THE PROMISE: Report of the Dark Energy Task Force 2006: The South Pole Telescope (SPT) is a 10-meter submillimeter-wave telescope with a 1000-element bolometric focal plane array with channels at 90, 150, 220 and 270 GHz. It would conduct a deep, large solid angle (4000 square degree) galaxy- cluster survey using the Sunyaev-Zel’dovich ef- fect. About 20,000 clusters with masses greater than 2 × 10 14 solar masses are expected to be dis- covered. 5 clusters/square degree RESULTS SO FAR: SPT: about 0.3 clusters/square degree (4/40 sq deg in Staniszewski et al 2008, now ~260/1000 sq deg in pipeline/T. Stark) ACT: about 0.2 clusters/square degree (J. Sievers, priv. comm)

23. Planck launched 5/14-09 and works well:

26. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu ITP June 21, 2010 Galaxy clustering progress