1. NEUTRINOS IN COSMOLOGY STEEN HANNESTAD UNIVERSITY OF AARHUS ERICE, 17 SEPTEMBER 2005 e    

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. 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

6. SDSS SURVEY

8. 2dF POWER SPECTRUM

9. SDSS POWER SPECTRUM

10. 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

11. SDSS

12. 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

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

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

15. 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

16. 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.)

17. 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

18. 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

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

20. 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

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

22. 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 STH 20051.5 eV @ 95%WMAP, SDSS, SNI-A, H 0

23.  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

24. 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

25. 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!

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

27. w ALLOWED TO VARY w KEPT FIXED m ALLOWED TO VARY m KEPT FIXED

28. THE STRONG m -w DEGENERACY OCCURS BECAUSE OF  M WHEN m INCREASES,  M MUST ALSO INCREASE TO PRODUCE THE SAME MATTER SPECTRUM. FOR w = -1 THIS QUICKLY BECOMES INCOMPATIBLE WITH SNI-A DATA, BUT NOT IF w IS ALLOWED TO VARY FREELY

29. KNOP ET AL. ASTRO-PH/0309368 (SCP)

30. 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

31. 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

32. 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) AT PRESENT THERE IS NO SIGNIFICANT BOUND ON EXTRA THERMAL RELICS, EITHER AT BBN OR AT RECOMBINATION! STH 2005, IN PREPARATION See also: Crotty, Lesgourgues & Pastor ’03 STH ’03, Pierpaoli ’03, Barger et al. ’03

33. STERILE NEUTRINOS: WHAT ABOUT LSND?

34. 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

35. 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)

36. 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

37. 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!

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

39. 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 CONTRIBUTION TO DENSITY FREE-STREAMING LENGTH

40. 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) Similar bound can be obtained for pseudoscalars (such a axions) – STH, Mirizzi & Raffelt 2005 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

41. 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

42. VIEL ET AL. astro-ph/0501562 THE 2  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

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 SNLS, DARK ENERGY CAMERA, SNAP WEAK LENSING SURVEYS (Pan-STARRS 2006, LSST 2012) BETTER CMBR TEMPERATURE MEASUREMENTS SatellitesBalloonsInterferometers WMAP (ongoing)Boomerang (2002-2003)CBI (ongoing) Planck (2007)TopHat (ongoing)DASI (ongoing) CMBR POLARIZATION MEASUREMENTS SatellitesBalloons Ground WMAP (ongoing)Boomerang (2002-3)Polatron (ongoing) Planck (2007)DASI

44. CMB POLARIZATION ANISOTROPY MEASUREMENT Gives a new sequence of power spectra Dodelson & Hu ’01

45. PROJECTED OBSERVATIONAL ERRORS FOR MAP AND PLANCK WMAP FINAL DATA (4 YEARS) PLANCK (STARTING 2007)

46. SNAP SATELLITE http://snap.lbl.gov THE SUPERNOVA ACCELERATION PROBE (SNAP) WILL OBSERVE ROUGHLY 2000 TYPEI-a SN OUT TO REDSHIFTS OF ORDER 1.5, STARTING FROM ~ 2012?

47. Distortion of background images by foreground matter UnlensedLensed WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE

48. FROM A WEAK LENSING SURVEY THE ANGULAR POWER SPECTRUM CAN BE CONSTRUCTED, JUST LIKE IN THE CASE OF CMB MATTER POWER SPECTRUM (NON-LINEAR) WEIGHT FUNCTION DESCRIBING LENSING PROBABILITY (SEE FOR INSTANCE JAIN & SELJAK ’96, ABAZAJIAN & DODELSON ’03, SIMPSON & BRIDLE ’04)

49. Non- linear physics Wide survey WEAK LENSING POWER SPECTRUM FIRST PROJECT Pan-STARRS WILL START IN JANUARY 2006

50. MASS BOUNDS ON LIGHT PARTICLES WILL IMPROVE SIGNIFICANTLY IN THE FUTURE, PERHAPS EVEN TO 0.1 eV FOR THE SUM OF NEUTRINO MASSES