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N EUTRINO C OSMOLOGY

N EUTRINO C OSMOLOGY. n e n m n t. STEEN HANNESTAD UNIVERSITY OF AARHUS COPENHAGEN, 17 DECEMBER 2005. NEUTRINOS, THE MICROWAVE BACKGROUND, AND LARGE SCALE STRUCTURE. WMAP 1-YEAR DATA. BOOMERANG 2003 FLIGHT – PUBLISHED DATA IN JULY 2005. ASTRO-PH/0507494. SDSS SURVEY.

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N EUTRINO C OSMOLOGY

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  1. NEUTRINO COSMOLOGY ne nm nt STEEN HANNESTAD UNIVERSITY OF AARHUS COPENHAGEN, 17 DECEMBER 2005

  2. NEUTRINOS, THE MICROWAVE BACKGROUND, AND LARGE SCALE STRUCTURE

  3. WMAP 1-YEAR DATA

  4. BOOMERANG 2003 FLIGHT – PUBLISHED DATA IN JULY 2005 ASTRO-PH/0507494

  5. SDSS SURVEY

  6. SDSS POWER SPECTRUM

  7. DATA FROM THE LYMAN-ALPHA FOREST PROVIDES AN INDEPENDENT MEASUREMENT OF POWER ON SMALL SCALES, BUT IN THE SEMI-LINEAR REGIME (CROFT ET AL. 2002, MCDONALD ET AL. 2003). THE RELIABILITY OF THE INFERRED MATTER SPECTRUM IS CONTROVERSIAL! CROFT ET AL. DATA

  8. SDSS

  9. THE SDSS MEASUREMENT OF BARYON OSCILLATIONS IN THE POWER SPECTRUM PROVIDE A FANTASTICALLY PRECISE MEASURE OF THE ANGULAR DISTANCE SCALE AND SETS COMPLEMENTARY LIMITS ON W AND w EISENSTEIN ET AL. 2005 (SDSS)

  10. SO, WHAT ABOUT NEUTRINO PHYSICS? NEUTRINO MASS HIERARCHY AND MIXING MATRIX ABSOLUTE NEUTRINO MASSES STERILE NEUTRINOS (LEPTOGENESIS) NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY

  11. THE NEUTRINO MASS MATRIX (WITH ONLY ACTIVE SPECIES) FLAVOUR (INTERACTION) STATES MASS (PROPAGATION) STATES 3 x 3 UNITARY MATRIX ETC

  12. STATUS OF 1-2 MIXING (SOLAR + KAMLAND) Araki et al. hep-ex/0406035

  13. STATUS OF 2-3 MIXING (ATMOSPHERIC + K2K) Maltoni et al. hep-ph/0405172

  14. If neutrino masses are hierarchical then oscillation experiments do not give information on the absolute value of neutrino masses ATMO. n K2K SOLAR n KAMLAND Normal hierarchy Inverted hierarchy However, if neutrino masses are degenerate no information can be gained from such experiments. Experiments which rely on the kinematics of neutrino mass are the most efficient for measuring m0 (or 0n2b decays)

  15. ”DEGENERATE NEUTRINO MASSES” FROM LESGOURGUES & PASTOR

  16. Tritium decay endpoint measurements have reached limits on the electron neutrino mass Mainz experiment, final analysis (Kraus et al.) This translates into a limit on the sum of the three mass eigenstates

  17. MEASUREMENT OF THE NEUTRINO MASS FROM TRITIUM DECAY FROM G. DREXLIN

  18. Neutrinoless double beta decay Only possible if neutrinos are massive Majorana particles 0:

  19. Ca 48 4271 0.187 4.10E24 2.52E16 Ge 76 2039 7.8 4.09E25 7.66E18 Se 82 2995 9.2 9.27E24 2.30E17 Zr 96 3350 2.8 4.46E24 5.19E16 Mo 100 3034 9.6 5.70E24 1.06E17 Pd 110 2013 11.8 1.86E25 2.51E18 Cd 116 2802 7.5 5.28E24 1.25E17 Sn 124 2288 5.64 9.48E24 5.93E17 Te 130 2529 34.5 5.89E24 2.08E17 Xe 136 2479 8.9 5.52E24 2.07E17 Nd 150 3367 5.6 1.25E24 8.41E15 Q-value (keV) (PS 0v)–1 (yrs x eV2) (PS 2v) –1 (yrs) Isotope Nat. abund. (%)

  20. THE HEIDELBERG – MOSCOW EXPERIMENT Heidelberg -Moscow • Five Ge diodes (overall mass 10.9 kg) • isotopically enriched ( 86%) in 76Ge • Lead box and nitrogen flushing of the detectors • Digital Pulse ShapeAnalysis (factor 5 reduction)Peak at 2039 keV

  21. Spectrum 0 peak region

  22. Latest HD-Moscow results Statistical significance: 54.98 kg x yr Including pulse shape analysis: 35.5 kg x yr (installed Nov. 95, only 4 detectors) T1/2 > 1.9 x 1025 yr (90% CL) m < 0.35 eV

  23. Heidelberg –Moscow evidence??? Evidence ? T1/2 = 0.6 - 8.4 x 1025 yr Subgroup of collaboration m = 0.17 - 0.63 eV H.V. Klapdor-Kleingrothaus et al, Phys. Lett. B 586, 198 (2004)

  24. THE ABSOLUTE VALUES OF NEUTRINO MASSES FROM COSMOLOGY NEUTRINOS AFFECT STRUCTURE FORMATION BECAUSE THEY ARE A SOURCE OF DARK MATTER HOWEVER, eV NEUTRINOS ARE DIFFERENT FROM CDM BECAUSE THEY FREE STREAM SCALES SMALLER THAN dFS DAMPED AWAY, LEADS TO SUPPRESSION OF POWER ON SMALL SCALES

  25. BY MEASURING THE MATTER POWER SPECTRUM 0 eV 0.3 eV T(k) = Transfer function IT IS POSSIBLE TO OBTAIN CONSTRAINTS ON mn 1 eV ROUGHLY ONE FINDS THAT EISENSTEIN, HU & TEGMARK ’99

  26. mn = 0 eV mn = 1 eV Ma ’96 mn = 7 eV mn = 4 eV

  27. WHILE NEUTRINO MASSES HAVE A PRONOUNCED INFLUENCE ON THE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMING SCALE THERE IS ONLY A VERY LIMITED EFFECT ON THE CMB

  28. COMBINED ANALYSIS OF CMB, 2dF AND LY-ALPHA DATA BY THE WMAP TEAM (Spergel et al. 2003)

  29. BOUND FROM SDSS + WMAP + BIAS + SDSS LYMAN ALPHA (SELJAK ET AL. ASTRO-PH/0407372) FOGLI ET AL. HEP-PH/0408045 FIND ~ 0.5 eV IN A SIMILAR STUDY BOTH RESULTS RELY ON THE ABILITY TO MEASURE THE EXACT MATTER FLUCTUATION AMPLITUDE ON SMALL SCALES THIS LOOKS VERY IMPRESSIVE, BUT IT NEEDS A REALITY CHECK!

  30. A SELECTION OF RECENT RESULTS ON Smn

  31. HEIDELBERG – MOSCOW FROM LESGOURGUES & PASTOR

  32. GENERAL HEALTH WARNING A GENERIC PROBLEM WITH USING COSMOLOGICAL OBSERVATIONS TO PROBE PARTICLE PHYSICS: IN GENERAL, LIKELIHOOD ANALYSES ARE CARRIED OUT ON TOP OF THE MINIMAL COSMOLOGICAL STANDARD MODEL HOWEVER, THERE COULD BE MORE THAN ONE NON-STANDARD EFFECT, SEVERELY BIASING THE PARAMETER ESTIMATE ANY DERIVED LIMIT SHOULD BE TREATED WITH SOME CARE!

  33. HOW CAN THE BOUND BE AVOIDED? CHANGE THE PRIMORDIAL SPECTRUM YES, BUT LEADS TO OTHER PROBLEMS TOPOLOGICAL DEFECTS? NO MAKE THE NEUTRINOS STRONGLY INTERACTING NO CHANGE THE DARK ENERGY EQUATION OF STATE YES (BUT NO) ……

  34. EXAMPLE: THERE IS A VERY STRONG DEGENERACY BETWEEN NEUTRINO MASS AND THE DARK ENERGY EQUATION OF STATE STH, ASTRO-PH/0505551 (PRL)

  35. BREAKING THE mn - w DEGENERACY WITHOUT USING THE LY-a • FOREST DATA: • USE WEAK LENSING (TALK BY HUITZU TU) • USE ANOTHER MEASURE OF THE ANGULAR SCALE • (BARYON ACOUSTIC OSCILLATION PEAK) • USING THE PRESENT SDSS DATA + CMB (WMAP, BOOMERANG) • + SNI-A (SNLS) DATA IT IS POSSIBLE TO DERIVE AN EXTREMELY • STRONG BOUND ON THE NEUTRINO MASS BECAUSE W AND w ARE • ESSENTIALLY FIXED

  36. 10 FREE PARAMETERS 10 FREE PARAMETERS 8 FREE PARAMETERS WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A, SDSS BARYONS WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A, SDSS BARYONS GOOBAR, HANNESTAD, MÖRTSELL, TU (IN PREPARATION) NO KNOWLEDGE OF THE BIAS OR LYMAN-ALPHA IS NEEDED FOR THIS BOUND!

  37. NEW BOUND FROM LESGOURGUES & PASTOR

  38. NEUTRINO MASS HIERARCHY AND MIXING MATRIX ABSOLUTE NEUTRINO MASSES STERILE NEUTRINOS NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY

  39. ANALYSIS OF ALL THE PRESENT DATA, INCLUDING BOOMERANG-03 GIVES A PRESENT LIMIT OF THIS IS ENTIRELY COMPATIBLE WITH THE MOST RECENT 4-HE DETERMINATION Cyburt et al. 2004 (astro-ph/0408033) STH 2005, JCAP 2006 AT PRESENT THERE IS NO SIGNIFICANT BOUND ON EXTRA THERMAL RELICS, EITHER AT BBN OR AT RECOMBINATION! See also: Crotty, Lesgourgues & Pastor ’03 STH ’03, Pierpaoli ’03, Barger et al. ’03

  40. WHAT ABOUT OTHER LIGHT, THERMALLY PRODUCED PARTICLES? ........... RADIONS AXINOS MAJORONS GRAVITONS AXIONS NEUTRINOS

  41. FOR ANY THERMALLY PRODUCED PARTICLE IT IS STRAIGHTFORWARD TO CALCULATE THE DECOUPLING EPOCH ETC. THE ONLY IMPORTANT PARAMETERS ARE AND WHERE g*IS THE EFECTIVE NUMBER OF DEGREES OF FREEDOM WHEN X DECOUPLES. CONTRIBUTION TO DENSITY FREE-STREAMING LENGTH

  42. Density bound for a Majorana fermion Based on WMAP, SDSS, SNI-a and Lyman-a data, No assumptions about bias! EW transition (~ 100 GeV) g* = 106.75 MASS BOUND FOR SPECIES DECOUPLING AROUND EW TRANSITION Below QCD transition (~ 100 MeV) g* < 20 DECOUPLING AFTER QCD PHASE TRANSITION LEADS TO STH, hep-ph/0409108 (See also STH & G Raffelt, JCAP 0404, 008) Similar bound can be obtained for pseudoscalars (such a axions) – STH, Mirizzi & Raffelt 2005

  43. NOTE THAT MASS BOUNDS CANNOT BE DIRECTLY EXTENDED TO RELIC PARTICLES WHICH MAKE UP MORE THAN A SMALL FRACTION OF THE TOTAL DENSITY!! LYMAN-ALPHA ANALYSIS IS BASED ON THE ASSUMPTION THAT THE POWER SPECTRUM IS CLOSE TO A POWER-LAW IF THERE IS EXPONENTIAL DAMPING THEN THE ”RAW” LYMAN-ALPHA DATA SHOULD BE USED DIRECTLY AND COMPARED WITH NUMERICAL SIMULATIONS THIS HAS BEEN DONE BY VIEL ET AL. astro-ph/0501562

  44. THE 2s LOWER BOUND ON THE MASS OF THE WDM PARTICLE IS ~ 500 eV THE BEST FIT IS NOT AT INFINITE MASS ALTHOUGH THE EFFECT IS NOT STATISTICALLY SIGNIFICANT VIEL ET AL. astro-ph/0501562

  45. WHAT IS IN STORE FOR THE FUTURE? BETTER CMB TEMPERATURE MEASUREMENTS Satellites Balloons Interferometers WMAP (ongoing)Boomerang CBI Planck (2007) Maxima, ArchaeopsDASI CMB POLARIZATION MEASUREMENTS Satellites Balloons Ground WMAP (ongoing)Boomerang Polatron Planck (2007) DASI LARGE SCALE STRUCTURE SURVEYS 2dF (completed) 250.000 galaxies SDSS (ongoing) 1.000.000 galaxies COSMOLOGICAL SUPERNOVA SURVEYS SNLS, DARK ENERGY CAMERA, SNAP WEAK LENSING SURVEYS (Pan-STARRS 2006, LSST 2012, …..)

  46. PROJECTED SENSITIVITIES FROM FUTURE EXPERIMENTS FROM LESGOURGUES & PASTOR

  47. THE KATRIN EXPERIMENT IN KARLSRUHE WILL MEASURE THE EFFECTIVE ELECTRON NEUTRINO MASS TO 0.2 eV (90%) BY USING TRITIUM DECAYS, STARTING IN 2008

  48. CONCLUSIONS NEUTRINO PHYSICS IS THE PRIME EXAMPLE OF HOW TO USE COSMOLOGY TO DO PARTICLE PHYSICS THE BOUND ON NEUTRINO MASSES IS ALREADY AN ORDER OF MAGNITUDE STRONGER THAN THAT FROM DIRECT EXPERIMENTS, ALBEIT MORE MODEL DEPENDENT WITHIN THE NEXT 5-10 YEARS THE MASS BOUND COULD REACH THE LEVEL NEEDED TO DETECT HIERARCHICAL NEUTRINO MASSES THE CLAIM FROM HEIDELBERG-MOSCOW WILL BE CHECKED

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