NEUTRINO PHYSICS FROM COSMOLOGY EVIDENCE FOR NEW PHYSICS? STEEN HANNESTAD, Aarhus University...
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Transcript of NEUTRINO PHYSICS FROM COSMOLOGY EVIDENCE FOR NEW PHYSICS? STEEN HANNESTAD, Aarhus University...
NEUTRINO PHYSICS FROM COSMOLOGYEVIDENCE FOR NEW PHYSICS?
STEEN HANNESTAD, Aarhus UniversityNuHorizons 2011
ne
nm
nt
Fermion Mass Spectrum
10 1001 10 1001 10 1001 10 1001 10 1001 1meV eV keV MeV GeV TeV
d s bQ = -1/3
u c tQ = +2/3
Charged Leptons e m t
All flavors
n3
Neutrinos
132313231223121323122312
132313231223121323122312
1313121312
ccescsscesccss
csesssccessccs
escscc
Uii
ii
i
1212
1212
sin
cos
s
c
)(
)(
)(
33
22
11
m
m
m
Ue
FLAVOUR STATES PROPAGATION STATES
MIXING MATRIX (UNITARY)
FORTUNATELY WE ONLY HAVE TO CARE ABOUT THE MASS STATES
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
LIGHTEST
INVERTED
NORMAL
HIERARCHICAL DEGENERATE
experimental observable is mn2
model independent neutrino mass from ß-decay kinematics
only assumption: relativistic energy-momentum relation
E0 = 18.6 keVT1/2 = 12.3 y
ß-decay and neutrino mass
T2:
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.)
em
TLK
KATRIN experiment
Karlsruhe Tritium Neutrino Experiment at Forschungszentrum KarlsruheData taking starting early 2012
25 m
eV 2.0~)(e
m
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
mh FROM K2
11
43/1
TT
N-BODY SIMULATIONS OF LCDM WITH AND WITHOUT NEUTRINO MASS (768 Mpc3) – GADGET 2
eV 9.6m 0m
T Haugboelle, University of Aarhus
256Mpc
AVAILABLE COSMOLOGICAL DATA
WMAP-7 TEMPERATURE POWER SPECTRUM
LARSON ET AL, ARXIV 1001.4635
LARGE SCALE STRUCTURE SURVEYS - 2dF AND SDSS
SDSS DR-7LRG SPECTRUM(Reid et al ’09)
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
n=0)
TOTFS
m
kkP
P
8~)(
0
NOW, WHAT ABOUT NEUTRINOPHYSICS?
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 44.0mUSING THE MINIMAL COSMOLOGICALMODEL
THERE ARE MANY ANALYSES IN THE LITERATURE
JUST ONE EXAMPLE
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
Gonzalez-Garcia et al., arxiv:1006.3795
WHAT IS Nn?
A MEASURE OF THE ENERGY DENSITY IN NON-INTERACTINGRADIATION IN THE EARLY UNIVERSE
THE STANDARD MODEL PREDICTION IS
3/4
0,0, 11
4
8
7 , 046.3
N
BUT ADDITIONAL LIGHT PARTICLES (STERILE NEUTRINOS,AXIONS, MAJORONS,…..) COULD MAKE IT HIGHER
Mangano et al., hep-ph/0506164
TIME EVOLUTION OFTHE 95% BOUND ONNn
ESTIMATED PLANCKSENSITIVITY
Pre-WMAP
WMAP-1
WMAP-3
WMAP-5
WMAP-7
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
Hamann, STH, Raffelt, Tamborra,Wong, arxiv:1006.5276 (PRL)
COSMOLOGY AT PRESENTNOT ONLY MARGINALLY PREFERS EXTRA ENERGYDENSITY, BUT ALSO ALLOWSFOR QUITE HIGH NEUTRINO MASSES!
3+N
N+3
See alsoDodelson et al. 2006Melchiorri et al. 2009Acero & Lesgourgues 2009
Updated Antineutrino mode MB results for E>475 MeV (official oscillation region)
• Results for 5.66E20 POT
• Maximum likelihood fit.• Null excluded at 99.4%
with respect to the two neutrino oscillation fit.
• Best Fit Point
(∆m2, sin2 2θ) =
(0.064 eV2, 0.96)
χ2/NDF= 16.4/12.6
P(χ2)= 20.5%• Results to be published.
E>475 MeV
Richard Van de Water, NEUTRINO 2010, June 14
A reanalysis of short baseline disappearance experiments seems to becompatible with oscillations (and requires at least one extra mass state)
Mention et al., arxiv:1101.2755
Hamann, STH, Raffelt, Wong(in preparation):
What happens to cosmologicalparameters if a prior is imposedon the neutrino mass?
(this is now done in an extendedmodel)
1s
2s
3s
BIG BANG NUCLEOSYNTHESIS
N n = 3
N n = 4
N n = 2
The helium production is very sensitive to Nn
Current helium data also suggests extra radiation
C.L.) (95% 14~ N
Aver et al 2010Izotov & Thuan 2010
WHAT IS IN STORE FOR THE FUTURE?
BETTER CMB TEMPERATURE AND POLARIZATIONMEASUREMENTS (PLANCK)
LARGE SCALE STRUCTURE SURVEYS AT HIGH REDSHIFT
MEASUREMENTS OF WEAK GRAVITATIONAL LENSINGON LARGE SCALES
Distortion of background images by foreground matter
Unlensed Lensed
WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE
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
drPa
gHC m
0
2
240 ),/(
)(
16
9
),/( rP
H
dng
0
''
)'()'(2)(
STH, TU, WONG 2006
EUCLIDESA M-CLASS MISSION2020-25
STH, TU & WONG 2006
THIS SOUNDS GREAT, BUT UNFORTUNATELY THE THEORETICIANSCANNOT JUST LEAN BACK AND WAIT FOR FANTASTIC NEW DATATO ARRIVE…..
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
-1
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
……………………..
mP
P
6.9~
FULL NON-LINEAR
mP
P
8~
LINEAR THEORY
Brandbyge, STH, Haugbølle, Thomsen, arXiv:0802.3700 (JCAP)Brandbyge & STH ’09, ’10 (JCAP), Viel, Haehnelt, Springel ’10
NON-LINEAR EVOLUTION PROVIDES AN ADDITIONAL AND VERY CHARACTERISTIC SUPPRESSION OF FLUCTUATION POWER DUE TO NEUTRINOS (COULD BE USED AS A SMOKING GUN SIGNATURE)
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 6.0m
INDIVIDUAL HALO PROPERTIES
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