1. NEUTRINOS IN NUCLEOSYNTHESIS AND STRUCTURE FORMATION STEEN HANNESTAD UNIVERSITY OF SOUTHERN DENMARK NOW2004, 17 SEPTEMBER 2004 e    

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

3. WMAP 1-YEAR DATA

4. 2dF Galaxy redshift survey 15 May 2002 0.5 1.0 1.5 2.0 2.5 Billion lightyears Redshift 0.1 0.2 0.3

5. SDSS SURVEY

7. 2dF POWER SPECTRUM

8. SDSS POWER SPECTRUM

9. 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

10. SDSS

11. EXPERIMENTAL QUESTIONS FROM NEUTRINO PHYSICS NEUTRINO MASS HIERARCHY AND MIXING MATRIX - solar & atmospheric neutrinos - supernovae ABSOLUTE NEUTRINO MASSES - cosmology: CMB and large scale structure - supernovae STERILE NEUTRINOS (LEPTOGENESIS) - cosmology, supernovae NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY - cosmology

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

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

14. Normal hierarchyInverted hierarchy If neutrino masses are hierarchical then oscillation experiments do not give information on the absolute value of neutrino masses 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 m 0 (or 0  decays) SOLAR KAMLAND ATMO. K2K TALKS BY FERUGLIO, GIUNTI

15. Tritium decay endpoint measurements have reached limits on the electron neutrino mass This translates into a limit on the sum of the three mass eigenstates Mainz experiment, final analysis (Kraus et al. 2003) TALKS BY GIUNTI, DREXLIN IF NEUTRINOS ARE MAJORANA PARTICLES, THEN 0 2  CAN OCCUR (TALKS BY FAESSLER, KLAPDOR-KLEINGROTHAUS)

16. 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 d FS DAMPED AWAY, LEADS TO SUPPRESSION OF POWER ON SMALL SCALES

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

18. m  eVm  eV m  eVm  eV Ma ’96

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

20. HOWEVER, THIS MASS LIMIT IS EXTREMELY DEPENDENT ON DATA OTHER THAN CMB, AND ON PRIORS. Elgaroy & Lahav (astro-ph/0303089, JCAP)

21. A SELECTION OF RECENT RESULTS ON  m WMAP ONLY13 eV @ 95%WMAP SPERGEL ET AL. (WMAP) 2003 0.69 eV @ 95%WMAP, CMB, 2dF,    H 0 STH 20031.01 eV @ 95%WMAP, CMB, 2dF, H 0 ALLEN, SMITH, BRIDLE 2003 eV @ 68%WMAP, CMB, 2dF,    H 0 TEGMARK ET AL 2003 1.8 eV @ 95%WMAP, SDSS BARGER ET AL 2003 0.65 eV @ 95%WMAP, CMB, 2dF, SDSS  H 0 CROTTY ET AL. 2004 1.0 eV @ 95%WMAP, CMB, 2dF, SDSS  H 0

22.  ANALYSIS WITH RECENT DATA: WMAP CMB DATA SDSS LARGE SCALE STRUCTURE DATA RIESS ET AL. SNI-a ”gold” SAMPLE Ly  DATA FROM KECK SAMPLE, NO PRIOR ON  8 (SMALL SCALE AMPLITUDE) STH, HEP-PH/0409108

23. 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

24. Fogli et al., hep-ph/0408045 hh Including the most recent Klapdor et al. constraint Klapdor-Kleingrothaus et al. Nucl. Inst. & Meth. A 522, 371 (2004) Phys. Lett. B 586, 198 (2004) leads to Normal hierarchy Inverted hierarchy

25. FINAL 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 A MODEL WITH BROKEN SCALE-INVARIANCE CAN ALLOW FOR A HIGH NEUTRINO MASS WHAT ABOUT TOPOLOGICAL DEFECTS? COULD WE EVEN BE LIVING IN A NEUTRINOLESS UNIVERSE? (BEACOM, BELL, DODELSON ASTRO-PH/0404585) ANY DERIVED LIMIT SHOULD BE TREATED WITH SOME CARE

26. EXPERIMENTAL QUESTIONS FROM NEUTRINO PHYSICS NEUTRINO MASS HIERARCHY AND MIXING MATRIX - solar & atmospheric neutrinos - supernovae ABSOLUTE NEUTRINO MASSES - cosmology: CMB and large scale structure - supernovae STERILE NEUTRINOS (LEPTOGENESIS) - cosmology, supernovae NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY - cosmology

27. ANALYSIS OF PRESENT DATA GIVES A LIMIT ON N OF NOTE THAT THIS MEANS A POSITIVE DETECTION OF THE COSMIC NEUTRINO BACK- GROUND AT 3.5  STH 2003 (JCAP 5, 004 (2003)) Because of the stringent bound from LEP on neutrinos lighter than about 45 GeV this bound is mainly of academic interest if all such light neutrinos couple to Z. However, sterile neutrinos can also contribute to N Crotty, Lesgourgues & Pastor ’03 Pierpaoli ’03, Barger et al. ’03

28. STERILE NEUTRINOS: WHAT ABOUT LSND?

29. TAKEN AT FACE VALUE THE WMAP RESULT ON NEUTRINO MASS SEEMS TO RULE OUT LSND BECAUSE NO ALLOWED REGIONS EXIST FOR LOW  m 2. (Pierce & Murayama, hep-ph/0302131; Giunti hep-ph/0302173) WMAP

30. HOWEVER, A DETAILED ANALYSIS SHOWS THAT INCREASING N, THE NEUTRINO MASS, AND THE MATTER DENSITY SIMULTANEOUSLY PRODUCES EXCELLENT FITS  0 = 1.0  M = 0.3  b = 0.05 H 0 = 70 n s = 1.0 m = 0 N = 3  0 = 1.0  M = 0.3  b = 0.05 H 0 = 70 n s = 1.0 m = 3eV N = 3  0 = 1.0  M = 0.3  b = 0.05 H 0 = 70 n s = 1.0 m = 3eV N = 8  0 = 1.0  M = 0.35  b = 0.05 H 0 = 70 n s = 1.0 m = 3eV N = 8 STH, JCAP 0305, 004 (2003), STH & G RAFFELT JCAP 0404, 008 (2004)

31. THE UPPER MASS LIMIT ON EACH INDIVIDUAL MASS EIGENSTATE IS ROUGHLY CONSTANT FOR ALL N IF ALL SPECIES CARRY EQUAL MASS STH & G RAFFELT (JCAP 0404, 008 (2004)) SEE ALSO CROTTY, LESGOURGUES & PASTOR HEP-PH/0402049

32. Maltoni, Schweitz, Tortola & Valle ’03 (hep-ph/0305312) ONLY IF LYMAN-ALPHA AND BIAS CONSTRAINTS ARE INCLUDED IS THE LSND SOLUTION EXCLUDED AT 95% C.L. (SELJAK ET AL. 2004) A GLOBAL ANALYSIS STILL LEAVES THE TWO LOWEST LYING ISLANDS IN PARAMETER SPACE FOR LSND!

33. BIG BANG NUCLEOSYNTHESIS THE WMAP+LSS LIMIT ON THE BARYON DENSITY CAN BE COMBARED TO THE CONFIDENCE REGION FROM OBSERVATIONS OF PRIMORDIAL DEUTERIUM THERE IS COMPLETE CONSIS- TENCY WITH THE DEUTERIUM VALUE! HOWEVER.... CYBURT, FIELDS & OLIVE, astro-ph/0302431

34. CYBURT, FIELDS & OLIVE, astro-ph/0302431 THERE IS AN INCONSISTENCY AT ROUGHLY 2  WITH HELIUM AND LITHIUM OBSERVATIONS

35. N  = 3 N  = 4 N  = 2 Helium-4 production is very sensitive to N BOUND ON THE RELATIVISTIC ENERGY DENSITY (NUMBER OF NEUTRINO SPECIES) FROM BBN

36. MOST RECENT RESULTS ON   FROM BBN BARGER ET AL. HEP-PH/0305075 CUOCO ET AL. ASTRO-PH/0307213 DIFFERENCES DUE TO ESTIMATED HELIUM UNCERTAINTY

37. 12-MIXING LEADS TO ALMOST COMPLETE FLAVOUR EQUILIBRATION BEFORE BBN AND SETS VERY STRINGENT BOUNDS ON THE MAGNITUDE OF THE CHEMICAL POTENTIAL Dolgov et al. ’02 Lunardini & Smirnov, hep-ph/0012056 (PRD), Dolgov et al., hep-ph/0201287 Abazajian, Beacom & Bell, astro-ph/0203442, Wong hep-ph/0203180 WHAT ABOUT NEUTRINO CHEMICAL POTENTIALS?

38. A GLOBAL FIT INCLUDING ALL DATA (BBN, WMAP, 2dF) YIELDS INDICATING THAT a)There seems to be a slight incon- sistency between BBN and CMB, meaning that either Y P is higher than usually believed, or N is lower than 3. b)There seem to be tight bounds on the presence of sterile neutrinos STH, JCAP 5, 004 (2003) COMBINING BBN, CMB AND LSS ALMOST IDENTICAL RESULT FOUND BY BARGER ET AL. hep-ph/0305075

39. NEUTRINO THERMALIZATION ALSO PROVIDES A VERY ROBUST LOWER BOUND ON THE REHEATING TEMPERATURE AT THE END OF INFLATION SEE ALSO: KAWASAKI ET AL. PRL 82, 4168 (1999) KAWASAKI ET AL. PRD 62, 023506 (2000) GIUDICE ET AL. PRD 64, 023508 (2001) GIUDICE ET AL. PRD 64, 043512 (2001) STH, PRD 70, 043506 (2004)

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

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

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

43. WHAT IS IN STORE FOR THE FUTURE? LARGE SCALE STRUCTURE SURVEYS 2dF (completed) 250.000 galaxies SDSS (ongoing) 1.000.000 galaxies COSMOLOGICAL SUPERNOVA SURVEYS SNAP satellite (2012???) WEAK LENSING SURVEYS BETTER CMBR TEMPERATURE MEASUREMENTS SatellitesBalloonsInterferometers WMAP (ongoing)Boomerang (ongoing)CBI (ongoing) Planck (2007)TopHat (ongoing)DASI (ongoing) CMBR POLARIZATION MEASUREMENTS SatellitesBalloons Ground WMAP (ongoing)Boomerang (2002-3)Polatron (ongoing) Planck (2007)DASI

44. MEASURING m USING CMB+LSS DATA SDSS-BRG

45. Lopez et al. 1998 PROSPECTS FOR FUTURE DETERMINATION OF N Data from Planck may allow for very accurate determination of N Standard model prediction N =3.03-3.04 due to heating and finite temperature effect could perhaps be detected

46. CONCLUSIONS ON NEUTRINOS USING PLANCK, SDSS AND WEAK LENSING SURVEYS IT WILL BE POSSIBLE TO PROBE MASSES AS SMALL AS 0.1-0.2 eV (FOR THE SUM OF ALL MASS EIGENSTATES). IT WILL BE POSSIBLE TO DETERMINE WHETHER NEUTRINO MASSES ARE HIERARCHICAL SIGNIFICANTLY BETTER THAN DIRECT MEASUREMENTS LIKE KATRIN, BUT ALSO LESS ROBUST THE EFFECTIVE NUMBER OF NEUTRINO SPECIES CAN BE PROBED WITH A PRECISION APPROACHING   CLOSE TO THE STANDARD MODEL PREDICTION OF 0.04 THE PRESENT UPPER BOUND ON THE NEUTRINO MASS IS SOMEWHERE IN THE REGION OF 0.5-1 eV