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NEUTRINO COSMOLOGY

NEUTRINO COSMOLOGY. n e n m n t. STEEN HANNESTAD UNIVERSITY OF AARHUS BLAUBEUREN, 3 JULY 2007. OUTLINE. A BRIEF REVIEW OF PRESENT COSMOLOGICAL DATA. BOUNDS ON NEUTRINO PROPERTIES. WHAT IS TO COME IN THE FUTURE?. THE COSMIC MICROWAVE BACKGROUND.

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NEUTRINO COSMOLOGY

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  1. NEUTRINO COSMOLOGY ne nm nt STEEN HANNESTAD UNIVERSITY OF AARHUS BLAUBEUREN, 3 JULY 2007

  2. OUTLINE A BRIEF REVIEW OF PRESENT COSMOLOGICAL DATA BOUNDS ON NEUTRINO PROPERTIES WHAT IS TO COME IN THE FUTURE?

  3. THE COSMIC MICROWAVE BACKGROUND WMAP TEMPERATURE MAP (ILC MAP) – March 2006

  4. WMAP-3 TEMPERATURE POWER SPECTRUM

  5. LARGE SCALE STRUCTURE SDSS SURVEY (1,000,000 galaxies)

  6. SDSS SPECTRUM TEGMARK ET AL. 2006 Astro-ph/0608632

  7. SLOAN DIGITAL SKY SURVEY FLY-THROUGH

  8. OTHER AVAILABLE STRUCTURE FORMATION DATA: THE BARYON ACOUSTIC PEAK (SDSS) – THE CMB OSCILLATION PATTERN SEEN IN BARYONS Eisenstein et al. 2005 THE LYMAN ALPHA FOREST (THE FLUX POWER SPECTRUM ON SMALL SCALES AT HIGH REDSHIFT) McDonald et al. astro-ph/0407377 (SDSS) Viel et al. WEAK GRAVITATIONAL LENSING Massey et al. 2007

  9. THE SDSS MEASUREMENT OF BARYON OSCILLATIONS IN THE POWER SPECTRUM PROVIDES A FANTASTICALLY PRECISE MEASURE OF THE ANGULAR DISTANCE SCALE AND TURNS OUT TO BE EXTREMELY USEFUL FOR PROBING NEUTRINO PHYSICS NEUTRINO MASSES ARE THE LARGEST SYSTEMATIC ERROR NOT ACCOUNTED FOR IN THE ANALYSIS EISENSTEIN ET AL. 2005 (SDSS)

  10. THE LYMAN-ALPHA FOREST AS A TOOL FOR MEASURING THE MATTER POWER SPECTRUM

  11. Ly-a forest analysis • Raw data: quasar spectra remove data not tracing (quasi-linear) Lya absorption • Flux power spectrum PF(k) hydrodynamical simulations + assumptions on thermodynamics of IGM • Linear power spectrum P(k)

  12. Power Spectrum of Cosmic Density Fluctuations SDSS BAO FROM MAX TEGMARK

  13. NEUTRINO PHYSICS

  14. STATUS OF 1-2 MIXING (SOLAR + KAMLAND) Strumia & Vissani hep-ph/0606054

  15. STATUS OF 2-3 MIXING (ATMOSPHERIC + K2K + MINOS) Strumia & Vissani hep-ph/0606054

  16. If neutrino masses are hierarchical then oscillation experiments do not give information on the absolute value of neutrino masses ATMO. n K2K MINOS 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 either the kinematics of neutrino mass or the spin-flip in neutrinoless double beta decay are the most efficient for measuring m0

  17. HIERARCHICAL DEGENERATE INVERTED NORMAL LIGHTEST

  18. Tritium decay endpoint measurements have provided 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

  19. THE ABSOLUTE VALUES OF NEUTRINO MASSES FROM COSMOLOGY NEUTRINOS AFFECT STRUCTURE FORMATION BECAUSE THEY ARE A SOURCE OF DARK MATTER FROM 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

  20. FINITE NEUTRINO MASSES SUPPRESS THE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMING LENGTH Sm = 0 eV Sm = 0.3 eV Sm = 1 eV

  21. N-BODY SIMULATIONS OF LCDM WITH AND WITHOUT NEUTRINO MASS (768 Mpc3) – GADGET 2 256 Mpc T Haugboelle, University of Aarhus

  22. WHAT IS THE PRESENT BOUND ON THE NEUTRINO MASS? WMAP-3 ONLY ~ 2.0 eV WMAP + LSS 0.68 eV COMPARE WITH WMAP-I: WMAP-1 ONLY ~ 2.1 eV WMAP + LSS ~ 0.7 eV (without information on bias) COMBINED ANALYSIS OF WMAP AND LSS DATA (Spergel et al. 2006)

  23. HOW CAN THE BOUND BE AVOIDED? THERE IS A VERY STRONG DEGENERACY BETWEEN NEUTRINO MASS AND THE DARK ENERGY EQUATION OF STATE WHEN CMB, LSS AND SNI-A DATA IS USED. THIS SIGNIFICANTLY RELAXES THE COSMOLOGICAL BOUND ON NEUTRINO MASS IF A LARGE NEUTRINO MASS IS MEASURED EXPERIMENTALLY THIS SEEMS TO POINT TO w < -1 STH, ASTRO-PH/0505551 (PRL) DE LA MACORRA ET AL. ASTRO-PH/0608351

  24. HOW CAN THE BOUND BE STRENGTHENED? MAKING THE BOUND SIGNIFICANTLY STRONGER REQUIRES THE USE OF OTHER DATA: EITHER ADDITIONAL DATA TO BREAK THE Wm – w DEGENERACY THE BARYON ACOUSTIC PEAK OR FIXING THE SMALL SCALE AMPLITUDE LYMAN – ALPHA DATA

  25. 10 FREE PARAMETERS 10 FREE PARAMETERS WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A, SDSS BARYONS GOOBAR, HANNESTAD, MÖRTSELL, TU (astro-ph/0602155, JCAP) USING THE BAO DATA THE BOUND IS STRENGTHENED, EVEN FOR VERY GENERAL MODELS BAO BAO+ LY-a LY-a No BAO 12 FREE PARAMETERS WMAP-3, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A, SDSS BAO WITH THE INCLUSION OF LYMAN-ALPHA DATA THE BOUND STRENGTHENS TO IN A SIMPLIFIED MODEL WITH 8 PARAMETERS VERY SIMILAR RESULTS HAVE SUBSEQUENTLY BEEN OBTAINED BY CIRELLI & STRUMIA AND FOGLI ET AL.

  26. SELJAK, SLOSAR & MCDONALD (ASTRO-PH/0604335) FIND IN THE SIMPLEST 8-PARAMETER MODEL FRAMEWORK WITH A NEW SDSS LYMAN-ALPHA ANALYSIS. NOTE, HOWEVER, THAT THIS DATA IS (EVEN MORE) INCOMPATIBLE WITH THE WMAP NORMALIZATION. VIEL ET AL. FIND A DIFFERENT NORMALIZATION BASED ON A DIFFERENT ANALYSIS OF THE SAME DATA. SELJAK, SLOSAR & MCDONALD SDSS LYMAN-ALPHA WMAP-3 NORMALIZATION

  27. SELJAK, SLOSAR & MCDONALD (ASTRO-PH/0604335) FIND IN THE SIMPLEST 8-PARAMETER MODEL FRAMEWORK WITH NEW SDSS LYMAN-ALPHA ANALYSIS. NOTE, HOWEVER, THAT THIS DATA IS (EVEN MORE) INCOMPATIBLE WITH THE WMAP NORMALIZATION. VIEL ET AL. FIND DIFFERENT NORMALIZATION BASED ON DIFFERENT ANALYSIS OF THE SAME DATA. GOOBAR, HANNESTAD, MORTSELL, TU (ASTRO-PH/0602155) SELJAK, SLOSAR & MCDONALD OLD SDSS LYMAN-ALPHA SDSS LYMAN-ALPHA NEW SDSS LYMAN-ALPHA VIEL ET AL. LYMAN-ALPHA WMAP-3 NORMALIZATION

  28. ADDITIONAL LIGHT DEGREES OF FREEDOM STH & RAFFELT (ASTRO-PH/0607101) ANALYSIS WITHOUT LYMAN-ALPHA COMPARISON WITH SH & RAFFELT ’04

  29. USING WMAP3+SDSS-LRG+SNI-A, WE FIND HAMANN, STH, RAFFELT, WONG arXiv:0705.0979 AT PRESENT THERE IS NO EVIDENCE FOR NON-STANDARD NEUTRINO PHYSICS THE CONSTRAINT IS COMPATIBLE WITH THE VALUE OBTAINED FROM BBN IS EXCLUDED AT ABOUT 5 SIGMA!

  30. WHAT ABOUT OTHER LIGHT, THERMALLY PRODUCED PARTICLES? 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

  31. An example: Thermally produced axions STH & Raffelt 04; STH, Mirizzi & Raffelt 05; Melchiorri, Mena & Slosar 07 Axions are thermalised mainly via axion-pion conversion With an interaction strength given by The axion mass is given by

  32. FOR AXIONS WITH STANDARD INTERACTIONS USING LYMAN-ALPHA DATA ARXIV:0705.2695 HAS DERIVED A MORE STRINGENT LIMIT (BECAUSE OF THE SAME DISCREPANCY BETWEEN CMB AND LYMAN-ALPHA AS FOR STANDARD NEUTRINOS) STH, Mirizzi & Raffelt, hep-ph/0504059

  33. THE BOUND ON THE AXION MASS SHOULD BE DERIVED ASSUMING A NON-ZERO NEUTRINO MASS (I.E. THE TWO PARAMETERS SHOULD BE FITTED TOGETHER) STANDARD AXION AXION-PION COUPLING CHANGED BY FACTOR STH, MIRIZZI, RAFFELT & WONG arXiv:0706.4198

  34. WHAT IS IN STORE FOR THE FUTURE? BETTER CMB TEMPERATURE AND POLARIZATION MEASUREMENTS (PLANCK) LARGE SCALE STRUCTURE SURVEYS AT HIGH REDSHIFT NEW SUPERNOVA SURVEYS MEASUREMENTS OF WEAK GRAVITATIONAL LENSING ON LARGE SCALES

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

  36. 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)

  37. WEAK LENSING HAS THE ADDED ADVANTAGE COMPARED WITH CMB THAT IT IS POSSIBLE TO DO TOMOGRAPHY BY MEASURING THE REDSHIFT OF SOURCE GALAXIES HIGH REDSHIFT LOW REDSHIFT

  38. THE SENSITIVITY TO NEUTRINO MASS WILL IMPROVE TO < 0.1 eV AT 95% C.L. USING WEAK LENSING COULD POSSIBLY BE IMPROVED EVEN FURTHER USING FUTURE LARGE SCALE STRUCTURE SURVEYS STH, TU & WONG 2006 (ASTRO-PH/0603019, JCAP)

  39. 95% CL STH, TU & WONG 2006

  40. WHY IS WEAK LENSING TOMOGRAPHY SO GOOD? IF MEASURED AT ONLY ONE REDSHIFT THE NEUTRINO SIGNAL IS DEGENERATE WITH OTHER PARAMETERS CHANGING DARK ENERGY EQUATION OF STATE INITIAL CONDITIONS WITH BROKEN SCALE INVARIANCE HOWEVER, BY MEASURING AT DIFFERENT REDSHIFTS THIS DEGENERACY CAN BE BROKEN

  41. Power spectrum suppression for a neutrino mass of 0.08 eV

  42. SENSITIVITY VS. DETECTION THRESHOLD FOR A SURVEY OF 1 GPC3 OUT TO A REDSHIFT OF 4 STH & Y. WONG, ASTRO-PH/0703031 NOTE THE HIGHLY NON-GAUSSIAN NATURE OF THE LIKELIHOOD CONTOURS

  43. ADVANTAGES OF PROBING STRUCTURE AT HIGH REDSHIFT STRUCTURES ARE MORE LINEAR VOLUME IS LARGER (THE HORIZON VOLUME IS ~ 1000 TIMES LARGER THAN THE SDSS-LRG VOLUME) HOW TO DO IT? LYMAN-ALPHA? BAO? (WFMOS) GALAXIES? (LSST) 21-CM? (SKA)

  44. z~1100 z~5 z~0.35

  45. COULD NEUTRINOS BE STRONGLY INTERACTING? BEACOM, BELL & DODELSON (2004) SUGGESTED A WAY TO EVADE THE COSMOLOGICAL NEUTRINO MASS BOUND: IF NEUTRINOS COUPLE STRONGLY ENOUGH WITH A MASSLESS SCALAR OR PSEUDO-SCALAR THEY CAN BE VERY MASSIVE, BUT HAVE NO EFFECT ON THE MATTER POWER SPECTRUM, EXCEPT FOR A SLIGHT SUPPRESSION DUE TO MORE RELATIVISTIC ENERGY DENSITY WHY? BECAUSE NEUTRINOS WOULD ANNIHILATE AND DISAPPEAR AS SOON AS THEY BECOME NON-RELATIVISTIC

  46. BEACOM, BELL & DODELSON 2004

  47. HOWEVER, NEUTRINOS WHICH ARE STRONGLY INTERACTING DURING RECOMBINATION ARE NOT AFFECTED BY SHEAR (EFFECTIVELY THEY BEHAVE LIKE A FLUID). THIS HAS IMPLICATIONS FOR CMB BECAUSE THE NEUTRINO POTENTIAL FLUCTUATIONS SOURCING THE CMB FLUCTUATIONS DO NOT DECAY THIS INCREASES THE CMB AMPLITUDE ON ALL SCALES SMALLER THAN THE HORIZON AT RECOMBINATION Strongly interacting neutrinos Standard model neutrinos Sth, astro-ph/0411475 (JCAP)

  48. SUCH STRONGLY INTERACTING NEUTRINOS ARE HIGHLY DISFAVOURED BY DATA (STH 04, BELL, PIERPAOLI & SIGURDSON 05 CIRELLI & STRUMIA 06, FRIEDLAND ET AL. 07) ALTHOUGH THE EXACT VALUE OF THE DISCREPANCY IS NOT FULLY SETTLED (but at least by Dc2 > 20 even with more d.o.f.) THIS CAN BE USED TO PUT THE STRONGEST KNOWN CONSTRAINTS ON NEUTRINO COUPLINGS TO MASSLESS SCALARS OR PSEUDOSCALARS (STH & RAFFELT HEP-PH/0509278 (PRD)) WE FIND Diagonal elements Off-diagonal elements FOR DERIVATIVE COUPLINGS THE BOUND WOULD BECOME EVEN STRONGER

  49. THE BOUND ON g CAN BE TRANSLATED INTO A BOUND ON THE NEUTRINO LIFETIME THIS BOUND FOR INSTANCE EXCLUDES THAT THERE SHOULD BE SIGNIFICANT NEUTRINO DECAY IN BEAMS FROM HIGH-ENERGY ASTROPHYSICAL SOURCES (STH & RAFFELT 2005)

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