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NEUTRINOS IN COSMOLOGY

NEUTRINOS IN COSMOLOGY. n e n m n t. STEEN HANNESTAD UNIVERSITY OF AARHUS ERICE, 17 SEPTEMBER 2005. NEUTRINOS, THE MICROWAVE BACKGROUND, AND LARGE SCALE STRUCTURE. WMAP 1-YEAR DATA. BOOMERANG 2003 FLIGHT – PUBLISHED DATA IN JULY 2005. ASTRO-PH/0507494.

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NEUTRINOS IN COSMOLOGY

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  1. NEUTRINOS IN COSMOLOGY ne nm nt STEEN HANNESTAD UNIVERSITY OF AARHUS ERICE, 17 SEPTEMBER 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. 2dF Galaxy redshift survey 15 May 2002 Redshift 0.1 0.2 0.3 0.5 1.0 1.5 2.0 2.5 Billion lightyears

  6. 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. 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. 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

  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 dFS DAMPED AWAY, LEADS TO SUPPRESSION OF POWER ON SMALL SCALES

  17. 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

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

  19. 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

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

  21. A SELECTION OF RECENT RESULTS ON Smn

  22. ANALYSIS WITH RECENT DATA: WMAP CMB DATA SDSS LARGE SCALE STRUCTURE DATA RIESS ET AL. SNI-a ”gold” SAMPLE Ly-a DATA FROM KECK SAMPLE, NO PRIOR ON s8(SMALL SCALE AMPLITUDE) S 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. 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!

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

  26. w ALLOWED TO VARY w KEPT FIXED mn ALLOWED TO VARY mn KEPT FIXED

  27. THE STRONG mn-w DEGENERACY OCCURS BECAUSE OF WM WHEN mn INCREASES, WM 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

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

  29. 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

  30. ANALYSIS OF PRESENT DATA GIVES A LIMIT ONNn OF NOTE THAT THIS MEANS A POSITIVE DETECTION OF THE COSMIC NEUTRINO BACK- GROUND AT 3.5s! Crotty, Lesgourgues & Pastor ’03 Pierpaoli ’03, Barger et al. ’03 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 Nn

  31. 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, IN PREPARATION 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

  32. STERILE NEUTRINOS: WHAT ABOUT LSND?

  33. WMAP TAKEN AT FACE VALUE THE WMAP RESULT ON NEUTRINO MASS SEEMS TO RULE OUT LSND BECAUSE NO ALLOWED REGIONS EXIST FOR LOW Dm2. (Pierce & Murayama, hep-ph/0302131; Giunti hep-ph/0302173)

  34. HOWEVER, A DETAILED ANALYSIS SHOWS THAT INCREASING Nn, THE NEUTRINO MASS, AND THE MATTER DENSITY SIMULTANEOUSLY PRODUCES EXCELLENT FITS W0 = 1.0 WM= 0.3Wb= 0.05H0 = 70 ns = 1.0 mn = 0 Nn = 3 W0 = 1.0 WM= 0.3 Wb= 0.05 H0 = 70 ns = 1.0 mn = 3eV Nn = 3 W0 = 1.0 WM= 0.3 Wb= 0.05 H0 = 70 ns = 1.0 mn = 3eV Nn = 8 W0 = 1.0 WM= 0.35 Wb= 0.05 H0 = 70 ns = 1.0 mn = 3eV Nn = 8 STH, JCAP 0305, 004 (2003), STH & G RAFFELT JCAP 0404, 008 (2004)

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

  36. A GLOBAL ANALYSIS STILL LEAVES THE TWO LOWEST LYING ISLANDS IN PARAMETER SPACE FOR LSND! 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)

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

  38. 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

  39. 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

  40. 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

  41. 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

  42. WHAT IS IN STORE FOR THE FUTURE? BETTER CMBR TEMPERATURE MEASUREMENTS Satellites Balloons Interferometers WMAP (ongoing)Boomerang (2002-2003)CBI (ongoing) Planck (2007) TopHat (ongoing)DASI (ongoing) CMBR POLARIZATION MEASUREMENTS Satellites Balloons Ground WMAP (ongoing)Boomerang (2002-3)Polatron (ongoing) 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)

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

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

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

  46. WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE Distortion of background images by foreground matter Unlensed Lensed

  47. 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)

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

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

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