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3 astrophysical measurements of neutrino mass

Nottingham. 3 astrophysical measurements of neutrino mass. Nov 17 ’04. Neutrino Mass. …and Mixing. Dave Wark. Imperial College/RAL.

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3 astrophysical measurements of neutrino mass

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  1. Nottingham 3 astrophysical measurements of neutrino mass Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL • Neutrino mass will tend to wash out intermediate scale structure during galaxy formation. Thus the presence of such structure in the present day distributions of galaxies disfavours neutrino mass. • The Z-burst model for the origin of supra-GZK cosmic rays requires a non-zero neutrino mass. • See hep-ph/0308168 for a method based on supernova neutrinos observed around a gravitational lens. It only requires you to see supernova neutrinos around a gravitational lens. That shouldn’t be too hard….

  2. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL 2dF Galaxy Redshift Survey

  3. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL

  4. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL P(k)=A kn T2(k) Neutrino Free Streaming DP(k)/P(k) = -8 Wn /Wm (Hu et al. 1998)

  5. Nottingham Nov 17 ’04 =0.01 =0.05 Neutrino Mass.. =0 …and Mixing Dave Wark Imperial College/RAL 2dF team: astro-ph/0204152 They derive mn,tot < 1.8 eV

  6. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL

  7. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL astro-ph/0302209

  8. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL astro-ph/0304237

  9. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL astro-ph/0306386

  10. Neutrino mass from Cosmology All upper limits 95% CL, but different assumed priors ! Slide from Ofer Lahav

  11. Nottingham Nov 17 ’04 Neutrino Mass.. …and Mixing Dave Wark Imperial College/RAL What does this mean for neutrino physics? • Sensitivity is better than tritium, and currently comparable to 0nbb decay – but clearly at this time suffers from substantial model dependencies. • Data improve with more MAP data, Planck, and the Sloan Digital Sky Survey, perhaps gaining another factor of 3-5 in potential sensitivity. (See astro-ph/0303344, which claims sn(mn) = 0.15 eV from Planck alone, and eventually perhaps 0.04 eV from better CMBR measurements) • What are the real model dependencies? Hubble parameter? Bias? What is a model-independent limit? Time will tell. Watch, or better yet, join in the fun. • Real connection between particle physics and cosmology!

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