1. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino (Mass) in Cosmology Thomas J. Weiler Vanderbilt University Nashville TN 37235, and CERN, Geneva, Switzerland

2. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Early-Universe Timeline

3. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Friedmann eqns, and energy partitions Omega So  behaves like a “matter” with 3p+  < 0 ! Can relate (F1) parameters to today’s values to write with “a” being the cosmic scale factor Inflation and data  Omega K ~ 0 Omega=  /  crit,  crit =6 protons/m 3

4. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino Decoupling Looking back, ’s last scattered at time t such that  DC ~ MeV, t ~ 1 s, z ~ 10 10. Coincidentally, T DC ~ T BBN ~ T e+e- vs. z eq = a 0 /a eq = Omega rad /Omega m ~ 4000, z recomb ~ 1100. Coincidentally, T eq ~ T recomb ~ eV ~ m i.e. G F 2 T 5 ~ T 2 /M P,

5. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino stat mech HDM models tried (top-down) Omega =1, i.e. each m ~30eV per flavor

6. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino density from BB photon density

7. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN n, n  >> any other density hadron wall? no wall a’tall sun SN87a Neutrino Incognito ~C B

8. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino time Liberated at T=Mev, t= 1 sec Depends on energy (Lorentz boost) Consider a 10 20 eV neutrino. Lorentz factor = 10 21 for m = 0.1 eV. Age of Uni is 10 18 sec, But age of is 10 18 /10 21 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched !

9. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN CR Spectrum above a TeV from Tom Gaisser VLHC (100 TeV) 2 50 Joules

10. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN BBN limits on N  and asymmetry Kneller & Steigman Competing effects: 1.Weak int’n rate equilibrates e +n  p+e -, as n/p ~ exp[-  m N /T DC ] ; So more e  less neutrons  less He/H 2.Expansion rate (monotonic with N ) decouples weak int’n; So more N  faster movie, earlier hotter T DC and more neutrons  more He/H H  S H, S = So one extra species is  S=0.08 Best fit is  N=0.25, L=2.5%

11. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Compensation and LSND Order 5% neutrino asymmetry -- to be contrasted with 10 -9 baryon asymmetry

12. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Four roads to absolute neutrino mass (SN discounted) 1. Tritium decay 2. 0v  decay 3. WMAP  LSS 4. Z-bursts on the relic C B

13. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Tritium decay limits on neutrino mass Q: Why tritium? A: It has a small Q-value, m T -(m D +m p +m e )

14. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN The oscillation “box” from a Feynman graph Where does the “mixing matrix” come in?

15. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN PMNS neutrino-mixing matrix Weak-interaction and mass “vectors” point differently: |n k >=U ki |n i >, or U ki = = *

16. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN e   Log m 2 m1m1 m3m3 m2m2  m 2 23 ~ 2.5 x 10 -3 eV 2  m 2 12 ~ 7 x 10 -5 eV 2 It “probably” looks something like this What we think we know about neutrino mass

17. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN e   Log m 2 m1m1 m3m3 m2m2 It looks like this m3m3 m2m2 m1m1 Or maybe …

18. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Naturalness may be over-rated Or a bug with a light-emitting tush? A rodent with a bill? Do these look natural?

19. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN 0  decay limits on neutrino mass

20. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino parameters: fundamental to physics, and a tool for astrophysics/cosmology As an astro tool, useful NOW (e.g. L e = L  = L  ) ; As a physics window, the view is unclear.

21. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN second task: decide whether contribute as Hot Dark Matter  [% of  cr ] neutrino masses and cosmology first task: bound mass

22. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Cosmic structure formation WMAP  2dF/SDSS *

23. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN COBE data *The raw temperature map (top) has a large diagonal asymmetry due to our motion with respect to the cosmic microwave background -a Doppler shift. *The temperature fluctuations after subtraction of the velocity contribution, showing primordial fluctuations and a large radio signal from nearby sources in our own galaxy (the horizontal strip). *The primordial fluctuations after subtraction of the galaxy signal. V

24. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN WMAP data The Universe at t recombination, ~ t equality

25. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN 2dF Galaxy Redshift Survey Peak from horizon scale at t eq HDM contributes to suppression of Small scales

26. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Today k > k nr ~ (Omega /Omega m ) 1/2 Omega m New length scale from neutrino mass LSS WMAP LSS formation is a battle between attractive gravity and repulsive pressure; the battle-line is the “Jean’s length” (4  G  /v s 2 ) 1/2 ~ (4  G/p) 1/2. The

27. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Tegmark cosmic cinema - CDM http://www.hep.upenn.edu/~max/cmb/movies.html Increasing the total density of matter (baryons + cold dark matter) pushes the epoch of matter-radiation equality back in time and moves the peak scale (the horizion size at that time) to the right.

28. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Tegmark cosmic cinema - HDM Increasing the density of massive neutrinos suppresses all scales smaller than a certain cutoff, which in turn shifts to the left as you increase the neutrino mass (and density)

29. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Tegmark cosmic cinema – more HDM If a CMB theorist gloats that he or she can measure the neutrino density, make sure to point out that galaxy surveys are much more sensitive.

30. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN A little HDM history

31. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino fits Elgaroy and Lahav

32. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN SDSS (Seljak et al) Increasing nu mass increases CMB spectrum, But decreases matter power spectrum ??

33. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Role of priors (Elgaroy and Kahav) Elgaroy and Lahav

34. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Resonant Neutrino Annihilation Mean-Free-Path Fig: Fargion, Mele, Salis  n     D H /h 70

35. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Escher’s “Angels and Devils” The early Uni was denser, more absorbing.

36. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino mass-spectroscopy: absorption and emission

37. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Z-bursts  Mpc TJW, 1982; Revival – 1997

38. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN - mass spectroscopy z max =2, 5, 20 (top to bottom), n-  =2 (bottom-up acceleration) Eberle, Ringwald, Song, TJW, 2004

39. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Dips & sobering realism hidden M X =4 10 14 and 10 16 GeV, to explain >GZK w/ Z-bursts; mass = 0.2 (0.4) eV - dashed (solid); Error bars – per energy decade, by 2013, for flux saturating present limits

40. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN The GZK puzzle

41. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Z-burst spectrum

42. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Fitted Z-burst (Emission) Flux Gelmini, Varieschi, TJW

43. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Nu-mass limit for Z-burst fitted to EECRs Gelmini, Varieschi, TJW

44. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger

45. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN “clear moonless nights”

46. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN See-saw (Leptogenesis to follow)

47. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Leptogenesis Three Sakharov conditions for Violate baryon number (B- L conserved => Baryogenesis:  B (=  L) nonzero 2.Violate C and CP  T (complex couplings) 3.Out of Thermal Equilibrium (decouple at T > M so no Boltzmann suppression, then decay at T < M when over-abundant)

48. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Extra-dimensions and neutrino mass Right-handed “sterile” neutrinos may be our probe of extra-dimensions

49. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Summary: Neutrinos are a splendid example of the interplay among particle physics, astrophysics, and cosmology

50. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN

51. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN

52. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN The “Learned Plot” Oscillation phase is. ( L  m 2 / 4 E  Figure parameterized by  m 2 / (eV) 2

53. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino Decay -- Models, Signatures, and Reach P(survive)= e –t/  = e –(L/E)(m/  0 ) Beacom, Bell, Hooper, Pakvasa, TJW

54. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN The cosmic flavor-mixing thm If theta 32 is maximal (it is), And if Re(U e3 ) is minimal (it is), Then  and  equilibrate; Further, if initial e flux is 1/3 (as from pion-muon decay chain), Then all three flavors equilibrate. e :  :  = 1 : 1 : 1 at Earth (and deviations  new physics)

55. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN AMANDA/IceCube  event

56. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Flavor ratio  Topology ratio Map

57. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Sensitivity of 1 flavor-projection to MNS parameters

58. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN pseudo-Dirac masses and cosmic neutrinos

59. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Z-burst schematic

60. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Neutrino Mass tomography in the Local Super-galactic Cluster (Fodor, Katz, Ringwald)

61. SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN Integrated Sachs-Wolfe effect