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What can we learn about neutrinos from cosmology?

What can we learn about neutrinos from cosmology?. Credit: SDSS team, Andrew Hamilton Blame: Max Tegmark. What have we learned so far?. Flyabout + SDSS movie. Brief History of the Universe. Fluctuation generator. Fluctuation amplifier. Hot Dense Smooth.

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What can we learn about neutrinos from cosmology?

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  1. What can we learn about neutrinos from cosmology? Credit: SDSS team, Andrew Hamilton Blame: Max Tegmark

  2. What have we learned so far?

  3. Flyabout + SDSS movie

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

  5. To 0th order: Fluctuation generator Fluctuation amplifier Hot DenseSmooth H(z) Cool Rarefied Clumpy (Graphics from Gary Hinshaw/WMAP team) Cosmological functions (z), G(z,k), Ps(k), Pt(k)

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

  7. H = dlna/dt, H2   Assumes k=0 SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 Vanilla rules OK!

  8. Measuring clustering (That’s where the neutrino signal is)

  9. History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

  10. Boomzoom z = 1000

  11. Boomzoom z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  12. Boomzoom z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  13. Boomzoom z = 0 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  14. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  15. Cmbgg OmOl

  16. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  17. 000619 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

  18. 1parmovies LSS

  19. 1parmovies Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  20. 1parmovies CMB Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  21. History (Figure from Wayne Hu) (Figure from WMAP team)

  22. History

  23. History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

  24. Boomzoom Guth & Kaiser 2005, Science

  25. 1parmovies CMB Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  26. 1parmovies CMB Clusters LSS Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  27. Boomzoom Lyman Alpha Forest Simulation: Cen et al 2001 LyF Quasar You

  28. 1parmovies CMB Clusters LSS Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  29. 1parmovies CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  30. GRAVITATIONAL LENSING: A1689 imaged by Hubble ACS, Broadhurst et al 2004

  31. distortion Lensing

  32. 1parmovies CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  33. 000619 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

  34. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  35. Measuring cosmological parameters

  36. Neutrinos

  37. Boomzoom How neutrinos suppress cosmic fluctuation growth • If all the matter can cluster: da • If only a fraction W* can cluster: dap, where • p=[(1+24 W*)-1]/4≈ W*3/5 ≈ (1-fn)3/5 • (Bond, Efstathiou & Silk 1980) Net growth until today: atoday/aprimordial ≈ 4700p ≈ 4700 e-4fn Power suppression: P(k)/P(k)primordial ≈ e-8fn fn≈ ∑ mni /94.4 eV wdm ≈ ∑ mni /12 eV, So 1 eV cuts power in half. Distinguish neutrinos from dark energy by time and scale dependence.

  38. Cmbgg OmOl

  39. Cmbgg OmOl

  40. Cmbgg OmOl CMB

  41. Cmbgg OmOl CMB + P(k)

  42. Cmbgg OmOl CMB + P(k) + LyaF

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

  44. Boomzoom Now: • WMAP CMB + SDSS gals & LyaF: ∑ mni < 0.4 eV Seljak et al, astro-ph/0407372, Goobar et al astro-ph/0602155 Future: • Planck CMB + LSST lensing: s(∑ mni) ~ 0.04 eV E.g., Hu & Tegmark astro-ph/9811168, Hu astro-ph/9904153, Hannestad et al, astro-ph/0603019

  45. Galaxy clustering progress

  46. Why are LRGs so useful?

  47. SDSS sphere anim

  48. History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496 Last scattering surface

  49. Our observable universe LSS Last scattering surface

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