2. Neutrinos in cosmology Credit: SDSS team, Andrew Hamilton Blame: Max Tegmark

3. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 What have we learned so far?

4. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Flyabout + SDSS movie

5. Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy Brief History of the Universe 400

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

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

8. SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 H = dlna/dt, H 2   Assumes k=0 Vanilla rules OK!

9. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Measuring clustering (That’s where the neutrino signal is)

10. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

11. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom z = 1000

12. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

13. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

14. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001 z = 0

15. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 1par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/0207047 + updates CMB

16. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 000619 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

17. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 1par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/0207047 + updates CMB

18. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Measuring cosmological parameters

19. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006

20. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Neutrinos (Øisten Elgarøy will give much more detail on this on Thursday)

21. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom How neutrinos suppress cosmic fluctuation growth If all the matter can cluster:  a Net growth until today: a today /a primordial ≈ 4700 p ≈ 4700 e -4f Power suppression: P(k)/P(k) primordial ≈ e -8f  f ≈ ∑ m i /94.4 eV  dm ≈ ∑ m i /12 eV, So 1 eV cuts power in half. If only a fraction  * can cluster:  a p, where p=[(1+24  * )-1]/4≈  * 3/5 ≈ (1-f ) 3/5 (Bond, Efstathiou & Silk 1980) Distinguish neutrinos from dark energy by time and scale dependence.

22. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Cmbgg OmOl

23. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Cmbgg OmOl

24. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Cmbgg OmOl CMB

25. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Cmbgg OmOl CMB + P(k)

26. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Cmbgg OmOl CMB + Ly  F + P(k)

27. THE FUTURE It's tough to make predictions, especially about the future. Yogi Berra

28. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Boom zoom Now: WMAP CMB + SDSS gals & Ly  F: ∑ m i < 0.4 eV E.g., Hu & Tegmark, astro-ph/9811168, Hu, astro-ph/9904153, Hannestad et al, astro-ph/0603019 Planck CMB + LSST lensing:  (∑ m i ) ~ 0.04 eV Seljak et al, astro-ph/0407372, Goobar et al, astro-ph/0602155 Spergel et al, astro-ph/0603449 Seljak et al, astro-ph/0604335 (< 0.17 eV) Future:

29. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Hata Neutrin os Cosmo progress so far

30. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Hata Neutrin os Inverted Normal Lesgourges & Pastor, astro-ph/0603494

31. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Galaxy clustering progress

32. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 Why are LRGs so useful?

33. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 SDSS sphere anim

34. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

35. LSS Our observable universe

36. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS Quasars

37. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS LRG’s

38. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS Common galaxies

39. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS Common gals: too dense Quasars: too sparse LRG’s: just right! Why LRG’s are “Goldilocks galaxies”:

40. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS LRG’s Also more strongly clustered

41. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SNOW Stockholm, May 2, 2006 LSS Why LRG’s are “just right”: 60000 LRG’s have more statistical power than 2 million regular gals (Eisenstein et al 2005)