1. NEUTRINO MASS FROM LARGE SCALE STRUCTURE STEEN HANNESTAD CERN, 8 December 2008 e    

2. 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 either the kinematics of neutrino mass or the spin-flip in neutrinoless double beta decay are the most efficient for measuring m 0 SOLAR KAMLAND ATMO. K2K MINOS

3. LIGHTEST INVERTED NORMAL HIERARCHICALDEGENERATE Lesgourgues and Pastor 2006

4. 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 FROM

5. AVAILABLE COSMOLOGICAL DATA

6. WMAP-5 TEMPERATURE POWER SPECTRUM M NOLTA ET AL., arXiv:0803.0593

7. LARGE SCALE STRUCTURE SURVEYS - 2dF AND SDSS

8. SDSS SPECTRUM TEGMARK ET AL. 2006 astro-ph/0608632

9. S m = 0.3 eV FINITE NEUTRINO MASSES SUPPRESS THE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMING LENGTH S m = 1 eV S m = 0 eV P(k)/P(k,m 

10. EISENSTEIN ET AL. 2005 (SDSS) THE SDSS MEASUREMENT OF BARYON OSCILLATIONS IN THE POWER SPECTRUM PROVIDES PRECISE MEASURE OF THE ANGULAR DISTANCE SCALE AND TURNS OUT TO BE EXTREMELY USEFUL FOR PROBING NEUTRINO PHYSICS NEUTRINO MASSES IS A POTENTIALLY IMPOR- TANT SYSTEMATIC ERROR NOT ACCOUNTED FOR IN THE ANALYSIS GOOBAR, HANNESTAD, MÖRTSELL, TU 2006

11. Astro-ph/0807.3551 FIRST MEASUREMENT OF THE RADIAL BARYON ACOUSTIC FEATURE PROVIDES VERY PRECISE MEASUREMENT OF H(z)

12. NOW, WHAT ABOUT NEUTRINO PHYSICS?

13. WMAP-5 ONLY ~ 1.3 eV WMAP + OTHER 0.67 eV Komatsu et al., arXiv:0803.0547 WHAT IS THE PRESENT BOUND ON THE NEUTRINO MASS?

14. GOOBAR, HANNESTAD, MÖRTSELL, TU (JCAP 2006) 10 FREE PARAMETERS WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A 10 FREE PARAMETERS WMAP, BOOMERANG, CBI SDSS, 2dF SNLS SNI-A, SDSS BARYONS 12 FREE PARAMETERS WMAP-3, BOOMERANG, CBI SDSS, 2dF, HST SNLS SNI-A, SDSS BARYONS No BAO BAO LY-a BAO+ LY-a USING THE BAO DATA THE BOUND IS STRENGTHENED, EVEN FOR VERY GENERAL MODELS IN MORE RESTRICTED MODELS THE BOUND IS STRONGER (BUT BEWARE OF THE PARAMETER DEGENERACIES)

15. PRELIMINARY RESULT: WITH WMAP-5 AND RADIAL BAO ALONE ONE FINDS AN UPPER BOUND OF ~ 0.4 – 0.5 eV FOR THE SUM OF NEUTRINO MASSES (STH & HAUGBØLLE, ARXIV:0812.????) THIS IS A VERY ROBUST RESULT AND VERY INSENSITIVE TO MODEL SPACE SELECTION!

16. ADDITIONAL RELATIVISTIC ENERGY DENSITY COMPARISON WITH SH & RAFFELT ’04 COULD BY CAUSED BY A NUMBER OF DIFFERENT EFFECTS ADDITIONAL PARTICLE SPECIES DECAY OF HEAVY SPECIES NEUTRINO CHEMICAL POTENTIAL …..

17. USING WMAP3+SDSS-LRG+SNI-A HAMANN, STH, RAFFELT, WONG arXiv:0705.0979 (JCAP) IS EXCLUDED AT ABOUT 5 SIGMA! THIS RESULT IS CONSISTENT WITH WMAP-5 (WMAP-5 ONLY) ALSO DE BERNARDIS ET AL 2008, HAMANN, LESGOURGUES & MANGANO 2008 SELJAK, SLOSAR & MCDONALD 2007

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

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

20. 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)

21. STH, TU, WONG 2006

22. STH, TU & WONG 2006 (ASTRO-PH/0603019, JCAP) 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

23. FUTURE SURVEYS LIKE LSST WILL PROBE THE POWER SPECTRUM TO ~ 1-2 PERCENT PRECISION WE SHOULD BE ABLE TO CALCULATE THE POWER SPECTRUM TO AT LEAST THE SAME PRECISION! ”LSST” ERROR BARS

24. 512 h -1 Mpc z = 0 z = 4 EVOLUTION OF NEUTRINO DENSITY FIELD

25. FULL NON-LINEAR LINEAR THEORY Brandbyge, STH, Haugbølle, Thomsen, arXiv:0802.3700 (ApJ) NON-LINEAR EVOLUTION PROVIDES AN ADDITIONAL AND VERY CHARACTERISTIC SUPPRESSION OF FLUCTUATION POWER DUE TO NEUTRINOS (COULD BE USED AS A SMOKING GUN SIGNATURE)

26. LIGHT NEUTRINOS ARE ALMOST IMPOSSIBLE TO FOLLOW AT HIGH Z BECAUSE OF THERMAL NOISE SOLUTION: FOLLOW NEUTRINOS USING LINEAR THEORY WITH A GRID-BASED METHOD, SIMULTANEOUSLY WITH THE CDM / BARYON N-BODY SOLVER BRANDBYGE & STH 2008 (IN PREPARATION) DIFFERENCE BETWEEN GRID AND PARTICLE METHOD

27. THIS METHOD WORKS FOR REALISTIC NEUTRINO MASSES (BELOW 0.5-0.6 eV) AT BETTER THAN 0.5% PRECISION THE COMPUTATIONAL SPEED IS ESSENTIALLY THE SAME AS FOR A PURE CDM SIMULATION (FACTOR ~ 10 OR MORE FASTER THAN WITH NEUTRINOS AS PARTICLES)

28. THE GRID METHOD IS NOT USEFUL FOR CALCULATING THE LOCAL RELIC NEUTRINO DENSITY FOR THIS THE 1-PARTICLE BOLTZMANN EQUATION SHOULD BE USED (RINGWALD & WONG 2004, STH, RINGWALD, TU & WONG 2005) CDM -PARTICLE -GRID z = 49 z = 4 z = 0 z = 49 z = 4 z = 0

29. WONG 2008 FOR RELATIVELY SMALL NEUTRINO MASSES THE RESULTS CAN BE REPRODUCED USING HIGHER ORDER PERTURBATION THEORY FOR SCALES UP TO k ~ 0.1 h / Mpc (SAITO ET AL. 2008, WONG 2008) THESE CALCULATIONS ALSO ASSUME THAT NEUTRINO STRUCTURES ARE LINEAR

30. CONCLUSIONS NEUTRINO PHYSICS IS PERHAPS THE PRIME EXAMPLE OF HOW TO USE COSMOLOGY TO DO (ORDINARY) PARTICLE PHYSICS THE BOUND ON NEUTRINO MASSES IS SIGNIFICANTLY STRONGER THAN WHAT CAN BE OBTAINED FROM DIRECT EXPERIMENTS, ALBEIT MUCH MORE MODEL DEPENDENT FUTURE OBSERVATIONS WILL CONTINUE TO IMPROVE THE SENSITIVITY TO NEUTRINO PROPERTIES