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NEUTRINO PHYSICS AND COSMOLOGY

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NEUTRINO PHYSICS AND COSMOLOGY. n e n m n t. STEEN HANNESTAD, Aarhus University BLOIS, 31 MAY 2012. FLAVOUR STATES. PROPAGATION STATES. MIXING MATRIX (UNITARY). LATE-TIME COSMOLOGY IS (ALMOST) INSENSITIVE TO THE MIXING STRUCTURE. - PowerPoint PPT Presentation
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NEUTRINO PHYSICS AND COSMOLOGY STEEN HANNESTAD, Aarhus University BLOIS, 31 MAY 2012 n e n m n t
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Page 1: NEUTRINO PHYSICS  AND COSMOLOGY

NEUTRINO PHYSICS AND COSMOLOGY

STEEN HANNESTAD, Aarhus UniversityBLOIS, 31 MAY 2012

ne

nm

nt

Page 2: NEUTRINO PHYSICS  AND COSMOLOGY

132313231223121323122312

132313231223121323122312

1313121312

ccescsscesccsscsesssccessccsescscc

Uii

ii

i

1212

1212

sin

cos

s

c

)()()(

33

22

11

mmm

Ue

nnn

nnn

t

m

FLAVOUR STATES PROPAGATION STATES

MIXING MATRIX (UNITARY)

LATE-TIME COSMOLOGY IS (ALMOST) INSENSITIVE TO THE MIXING STRUCTURE

Page 3: NEUTRINO PHYSICS  AND COSMOLOGY

Normal hierarchy Inverted hierarchy

If neutrino masses are hierarchical then oscillation experimentsdo 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 massor the spin-flip in neutrinoless double beta decay are the most efficient for measuring m0

catmospherimm 0

SOLAR nKAMLAND

ATMO. nK2KMINOS

Page 4: NEUTRINO PHYSICS  AND COSMOLOGY

LIGHTEST

INVERTED

NORMAL

HIERARCHICAL DEGENERATE

Page 5: NEUTRINO PHYSICS  AND COSMOLOGY

experimental observable is mn2

model independent neutrino mass from ß-decay kinematicsonly assumption: relativistic energy-momentum relation

E0 = 18.6 keVT1/2 = 12.3 y

ß-decay and neutrino mass

T2:

Page 6: NEUTRINO PHYSICS  AND COSMOLOGY

Tritium decay endpoint measurements have provided limitson the electron neutrino mass

This translates into a limit on the sum of the three mass eigenstates

(95%) eV 3.22/1

22 iei mU

eV 7im

Mainz experiment, final analysis (Kraus et al.)

emn

Page 7: NEUTRINO PHYSICS  AND COSMOLOGY

TLK

KATRIN experiment

Karlsruhe Tritium Neutrino Experiment at Forschungszentrum KarlsruheData taking starting 2013

25 m

eV 2.0~)(e

mn

Page 8: NEUTRINO PHYSICS  AND COSMOLOGY

NEUTRINO MASS AND ENERGY DENSITYFROM COSMOLOGY

NEUTRINOS AFFECT STRUCTURE FORMATIONBECAUSE THEY ARE A SOURCE OF DARK MATTER(n ~ 100 cm-3)

HOWEVER, eV NEUTRINOS ARE DIFFERENT FROM CDM BECAUSE THEY FREE STREAM

1eVFS Gpc 1~ md

SCALES SMALLER THAN dFS DAMPED AWAY, LEADS TOSUPPRESSION OF POWER ON SMALL SCALES

eV 932 n

n

mh FROM K2

114 3/1

n TT

Page 9: NEUTRINO PHYSICS  AND COSMOLOGY

N-BODY SIMULATIONS OF LCDM WITH AND WITHOUT NEUTRINO MASS (768 Mpc3) – GADGET 2

eV 9.6nm 0nm

T Haugboelle, University of Aarhus

256Mpc

Page 10: NEUTRINO PHYSICS  AND COSMOLOGY

AVAILABLE COSMOLOGICAL DATA

Page 11: NEUTRINO PHYSICS  AND COSMOLOGY

WMAP TEMPERATURE MAP

THE COSMIC MICROWAVE BACKGROUND

Page 12: NEUTRINO PHYSICS  AND COSMOLOGY

WMAP-7 TEMPERATURE POWER SPECTRUM

LARSON ET AL, ARXIV 1001.4635

ADDITIONAL DATA ON SMALLER SCALES FROM ATACAMA COSMOLOGY TELESCOPE (Dunkley et al. 2011)SOUTH POLE TELESCOPE (Keisler et al. 2011)

Page 13: NEUTRINO PHYSICS  AND COSMOLOGY

LARGE SCALE STRUCTURE SURVEYS - 2dF AND SDSS

Page 14: NEUTRINO PHYSICS  AND COSMOLOGY

SDSS DR-7LRG SPECTRUM(Reid et al ’09)

Page 15: NEUTRINO PHYSICS  AND COSMOLOGY

Sm = 0.3 eV

FINITE NEUTRINO MASSES SUPPRESS THE MATTER POWERSPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMINGLENGTH

Sm = 1 eV

Sm = 0 eV

P(k)

/P(k,m

n0

TOTFS

m

kkPP

n8~)(

0

Page 16: NEUTRINO PHYSICS  AND COSMOLOGY

NOW, WHAT ABOUT NEUTRINOPHYSICS?

Page 17: NEUTRINO PHYSICS  AND COSMOLOGY

WHAT IS THE PRESENT BOUND ON THE NEUTRINO MASS?

STH, MIRIZZI, RAFFELT, WONG (arxiv:1004:0695)HAMANN, STH, LESGOURGUES, RAMPF & WONG (arxiv:1003.3999)

DEPENDS ON DATA SETS USED AND ALLOWED PARAMETERS

C.L. 95 @ eV 44.0nmUSING THE MINIMAL COSMOLOGICALMODEL

THERE ARE MANY ANALYSES IN THE LITERATURE

JUST ONE EXAMPLE

Page 18: NEUTRINO PHYSICS  AND COSMOLOGY

THE NEUTRINO MASS FROM COSMOLOGY PLOT

Larger modelspace

More data

CMB only

+ SDSS

+ SNI-a+WL

+Ly-alpha

MinimalLCDM

+Nn +w+……

1.1 eV

0.6 eV

~ 0.5 eV

~ 0.2 eV

~ 2 eV 2.? eV ??? eV

~ 1 eV 1-2 eV

0.5-0.6 eV 0.5-0.6 eV

0.2-0.3 eV 0.2-0.3 eV

Page 19: NEUTRINO PHYSICS  AND COSMOLOGY

Gonzalez-Garcia et al., arxiv:1006.3795

Page 20: NEUTRINO PHYSICS  AND COSMOLOGY

WHAT IS Nn?

A MEASURE OF THE ENERGY DENSITY IN NON-INTERACTINGRADIATION IN THE EARLY UNIVERSE

THE STANDARD MODEL PREDICTION IS

nn

n 3/4

0,0, 11

487 , 046.3

N

BUT ADDITIONAL LIGHT PARTICLES (STERILE NEUTRINOS,AXIONS, MAJORONS,…..) COULD MAKE IT HIGHER

Mangano et al., hep-ph/0506164

Page 21: NEUTRINO PHYSICS  AND COSMOLOGY

TIME EVOLUTION OFTHE 95% BOUND ONNn

ESTIMATED PLANCKSENSITIVITY

Pre-WMAP

WMAP-1

WMAP-3

WMAP-5

WMAP-7

Page 22: NEUTRINO PHYSICS  AND COSMOLOGY

ASSUMING A NUMBER OF ADDITIONAL STERILE STATES OF APPROXIMATELY EQUAL MASS, TWO QUALITATIVELY DIFFERENTHIERARCHIES EMERGE

3+N N+3

ns

nsnA

nA

A STERILE NEUTRINO IS PERHAPS THE MOST OBVIOUS CANDIDATEFOR AN EXPLANATION OF THE EXTRA ENERGY DENSITY

Page 23: NEUTRINO PHYSICS  AND COSMOLOGY

HOW DO THESE TWO HINTS FIT TOGETHER? CAN THEY BE EXPLAINED BY THE SAME PHYSICS?

SHORT ANSWER: IT IS DIFFICULT WITHOUT MODIFYING COSMOLOGY

MODIFYING FOR EXAMPLE THE DARK ENERGY EQUATION OF STATE CAN HELP, BUT THE 3+2 MODEL IS STRONGLY DISFAVOURED

THE 3+1 MODEL PROVIDES AS GOOD A FIT AS STANDARD LCDM(Hamann, STH, Raffelt, Wong 2011)

Page 24: NEUTRINO PHYSICS  AND COSMOLOGY

WHAT IS IN STORE FOR THE FUTURE?

BETTER CMB TEMPERATURE AND POLARIZATIONMEASUREMENTS (PLANCK)

LARGE SCALE STRUCTURE SURVEYS AT HIGHER REDSHIFT AND IN LARGER VOLUMES

MEASUREMENTS OF WEAK GRAVITATIONAL LENSINGON LARGE SCALES

Page 25: NEUTRINO PHYSICS  AND COSMOLOGY

Distortion of background images by foreground matter

Unlensed Lensed

WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE

Page 26: NEUTRINO PHYSICS  AND COSMOLOGY

FROM A WEAK LENSING SURVEY THE ANGULAR POWER SPECTRUMCAN BE CONSTRUCTED, JUST LIKE IN THE CASE OF CMB

MATTER POWER SPECTRUM (NON-LINEAR)

WEIGHT FUNCTION DESCRIBING LENSINGPROBABILITY

(SEE FOR INSTANCE JAIN & SELJAK ’96, ABAZAJIAN & DODELSON ’03,SIMPSON & BRIDLE ’04)

H

drPagHC m

0

224

0 ),/()(169

),/( rP

H

dng

0

''

)'()'(2)(

Page 27: NEUTRINO PHYSICS  AND COSMOLOGY

STH, TU, WONG 2006

Page 28: NEUTRINO PHYSICS  AND COSMOLOGY

EUCLIDESA M-CLASS MISSION2019SELECTED OCTOBER 2011

Page 29: NEUTRINO PHYSICS  AND COSMOLOGY

THE EUCLID MISSION

Page 30: NEUTRINO PHYSICS  AND COSMOLOGY

EUCLID WILL FEATURE:

A WEAK LENSING MEASUREMENT OUT TO z ~ 2, COVERINGAPPROXIMATELY 20,000 deg2 (THIS WILL BE MAINLY PHOTOMETRIC)

A GALAXY SURVEY OF ABOUT few x 107 GALAXIES (75 x SDSS)

A WEAK LENSING BASED CLUSTER SURVEY

Page 31: NEUTRINO PHYSICS  AND COSMOLOGY

z~0.35

z~1100

z~2

Page 32: NEUTRINO PHYSICS  AND COSMOLOGY

STH, TU & WONG 2006

EUCLID WL

HAMANN, STH, WONG 12: COMBINING THE EUCLID WL AND GALAXYSURVEYS WILL ALLOW FOR A 3-4 DETECTION OF THE NORMAL HIERARCHY

Page 33: NEUTRINO PHYSICS  AND COSMOLOGY

THIS SOUNDS GREAT, BUT UNFORTUNATELY THE THEORETICIANSCANNOT JUST LEAN BACK AND WAIT FOR FANTASTIC NEW DATATO ARRIVE…..

Page 34: NEUTRINO PHYSICS  AND COSMOLOGY

FUTURE SURVEYS LIKE EUCLID 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

-1

Page 35: NEUTRINO PHYSICS  AND COSMOLOGY

IN ORDER TO CALCULATE THE POWER SPECTRUM TO 1%ON THESE SCALES, A LARGE NUMBER OF EFFECTS MUST BE TAKEN INTO ACCOUNT

BARYONIC PHYSICS – STAR FORMATION, SN FEEDBACK,…..

NEUTRINOS, EVEN WITH NORMAL HIERARCHY

NON-LINEAR GRAVITY

……………………..

Page 36: NEUTRINO PHYSICS  AND COSMOLOGY

mPP

n6.9~

FULL NON-LINEAR

mPP

n8~

LINEAR THEORY

Brandbyge, STH, Haugbølle, Thomsen ’08Brandbyge & STH ’09, ’10, Viel, Haehnelt, Springel ’10STH, Haugbølle & Schultz ’12, Wagner, Verde & Jimenez ’12

NON-LINEAR EVOLUTION PROVIDES AN ADDITIONAL SUPPRESSION OF FLUCTUATION POWER IN MODELS WITH MASSIVE NEUTRINOS

Page 37: NEUTRINO PHYSICS  AND COSMOLOGY

sunM14105

CDM n

1 < p/T < 20 < p/T < 1 2 < p/T < 3

3 < p/T < 4 4 < p/T < 5 5 < p/T < 6

512 h-1 Mpc

eV 6.0nm

INDIVIDUAL HALO PROPERTIES

Page 38: NEUTRINO PHYSICS  AND COSMOLOGY

CONCLUSIONS

NEUTRINO PHYSICS IS PERHAPS THE PRIME EXAMPLE OF HOW TO USE COSMOLOGY TO DO PARTICLE PHYSICS

THE BOUND ON NEUTRINO MASSES IS SIGNIFICANTLYSTRONGER THAN WHAT CAN BE OBTAINED FROM DIRECT EXPERIMENTS, ALBEIT MUCH MORE MODEL DEPENDENT

COSMOLOGICAL DATA MIGHT ACTUALLY BE POINTING TO PHYSICS BEYOND THE STANDARD MODEL IN THE FORM OFSTERILE NEUTRINOS

NEW DATA FROM PLANCK AND EUCLID WILL PROVIDE APOSITIVE DETECTION OF A NON-ZERO NEUTRINO MASS


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