neutrinos in cosmology steen hannestad university of aarhus erice, 17 september 2005 e
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NEUTRINOS IN COSMOLOGY
STEEN HANNESTAD UNIVERSITY OF AARHUS
ERICE, 17 SEPTEMBER 2005
e
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NEUTRINOS, THE MICROWAVE BACKGROUND,AND LARGE SCALE STRUCTURE
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WMAP 1-YEAR DATA
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BOOMERANG 2003 FLIGHT – PUBLISHED DATA IN JULY 2005
ASTRO-PH/0507494
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2dF Galaxy redshift survey15 May 2002
0.5 1.0 1.5 2.0 2.5
Billion lightyears
Red
shift
0.1
0.
2
0.3
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SDSS SURVEY
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2dF POWER SPECTRUM
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SDSS POWER SPECTRUM
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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
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SDSS
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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
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Araki et al. hep-ex/0406035
STATUS OF 1-2 MIXING (SOLAR + KAMLAND)
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STATUS OF 2-3 MIXING (ATMOSPHERIC + K2K)
Maltoni et al. hep-ph/0405172
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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 the kinematics of neutrino massare the most efficient for measuring m0 (or 0 decays)
catmospherimm 0
SOLAR KAMLAND
ATMO. K2K
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Tritium decay endpoint measurements have reached 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 mUm
e
eV 7im
Mainz experiment, final analysis (Kraus et al.)
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THE ABSOLUTE VALUES OF NEUTRINO MASSESFROM COSMOLOGY
NEUTRINOS AFFECT STRUCTURE FORMATIONBECAUSE THEY ARE A SOURCE OF DARK MATTER
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
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mP
P
8
BY MEASURING THEMATTER POWER SPECTRUM
)()()( 0 kTkPkP
T(k) = Transfer functionIT IS POSSIBLE TO OBTAINCONSTRAINTS ON m
ROUGHLY ONE FINDS THAT
EISENSTEIN, HU & TEGMARK ’99
0.3 eV
1 eV
0 eV
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m eV m eV
m eV m eVMa ’96
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WHILE NEUTRINO MASSES HAVE A PRONOUNCED INFLUENCE ONTHE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THEFREE-STREAMING SCALE THERE IS ONLY A VERY LIMITED EFFECTON THE CMB
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COMBINED ANALYSIS OF CMB, 2dF AND LY-ALPHA DATA BY THEWMAP TEAM (Spergel et al. 2003)
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A SELECTION OF RECENT RESULTS ON m
WMAP ONLY 13 eV @ 95% WMAP
SPERGEL ET AL. (WMAP) 2003
0.69 eV @ 95% WMAP, CMB, 2dF, H0
STH 2003 1.01 eV @ 95% WMAP, CMB, 2dF, H0
ALLEN, SMITH, BRIDLE 2003
eV @ 68% WMAP, CMB, 2dF, H0
TEGMARK ET AL 2003
1.8 eV @ 95% WMAP, SDSS
BARGER ET AL 2003
0.65 eV @ 95% WMAP, CMB, 2dF, SDSS H0
CROTTY ET AL. 2004
1.0 eV @ 95% WMAP, CMB, 2dF, SDSS H0
STH 2005 1.5 eV @ 95% WMAP, SDSS,
SNI-A, H0
3.026.056.0
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ANALYSIS WITH RECENT DATA:WMAP CMB DATASDSS LARGE SCALE STRUCTURE DATARIESS ET AL. SNI-a ”gold” SAMPLE Ly DATA FROM KECK SAMPLE, NO PRIOR ON 8 (SMALL SCALE AMPLITUDE)
STH, HEP-PH/0409108
C.L. 95% @ eV 65.0 m
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BOUND FROM SDSS + WMAP + BIAS + SDSS LYMAN ALPHA(SELJAK ET AL. ASTRO-PH/0407372)
C.L. 95% @ eV 42.0 m
FOGLI ET AL. HEP-PH/0408045 FIND ~ 0.5 eV IN A SIMILAR STUDY
BOTH RESULTS RELY ON THE ABILITY TO MEASURE THEEXACT MATTER FLUCTUATION AMPLITUDE ON SMALLSCALES
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GENERAL HEALTH WARNING
A GENERIC PROBLEM WITH USING COSMOLOGICAL OBSERVATIONSTO PROBE PARTICLE PHYSICS:
IN GENERAL, LIKELIHOOD ANALYSES ARE CARRIED OUT ON TOPOF THE MINIMAL COSMOLOGICAL STANDARD MODEL
HOWEVER, THERE COULD BE MORE THAN ONE NON-STANDARDEFFECT, SEVERELY BIASING THE PARAMETER ESTIMATE
ANY DERIVED LIMIT SHOULD BE TREATED WITH SOME CARE!
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STH, ASTRO-PH/0505551
EXAMPLE:
THERE IS A VERY STRONG DEGENERACY BETWEEN NEUTRINOMASS AND THE DARK ENERGY EQUATION OF STATE
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w ALLOWED TO VARY
w KEPT FIXED
m ALLOWED TO VARY
m KEPT FIXED
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THE STRONG m-w DEGENERACY OCCURS BECAUSE OF M
WHEN m INCREASES, M MUST ALSO INCREASE TO PRODUCETHE SAME MATTER SPECTRUM.
FOR w = -1 THIS QUICKLY BECOMES INCOMPATIBLE WITH SNI-ADATA, BUT NOT IF w IS ALLOWED TO VARY FREELY
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KNOP ET AL. ASTRO-PH/0309368 (SCP)
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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
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ANALYSIS OF PRESENT DATAGIVES A LIMIT ON N OF
C.L.) (95% 72 N
NOTE THAT THIS MEANS APOSITIVE DETECTION OF THE COSMIC NEUTRINO BACK-GROUND AT 3.5
STH 2003 (JCAP 5, 004 (2003))
Because of the stringent bound from LEP on neutrinos lighter than about 45 GeV
008.0992.2 N
this bound is mainly of academic interest if all such light neutrinos couple to Z. However, sterile neutrinos can also contribute to N
Crotty, Lesgourgues & Pastor ’03Pierpaoli ’03, Barger et al. ’03
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ANALYSIS OF ALL THE PRESENTDATA, INCLUDING BOOMERANG-03GIVES A PRESENT LIMIT OF
C.L.) (95% 2.54.2 N
THIS IS ENTIRELY COMPATIBLEWITH THE MOST RECENT 4-HEDETERMINATION
0092.02495.0 YCyburt et al. 2004 (astro-ph/0408033)
AT PRESENT THERE IS NO SIGNIFICANT BOUND ON EXTRA THERMAL RELICS, EITHER AT BBN OR AT RECOMBINATION!
STH 2005, IN PREPARATION
See also: Crotty, Lesgourgues & Pastor ’03STH ’03, Pierpaoli ’03, Barger et al. ’03
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STERILE NEUTRINOS: WHAT ABOUT LSND?
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TAKEN AT FACE VALUE THE WMAP RESULT ON NEUTRINO MASSSEEMS TO RULE OUT LSND BECAUSE NO ALLOWED REGIONS EXISTFOR LOW m2. (Pierce & Murayama, hep-ph/0302131; Giunti hep-ph/0302173)
WMAP
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HOWEVER, A DETAILED ANALYSIS SHOWS THAT INCREASING N, THE NEUTRINO MASS, AND THE MATTER DENSITY SIMULTANEOUSLYPRODUCES EXCELLENT FITS
0 = 1.0 M= 0.3 b= 0.05 H0 = 70 ns = 1.0 m = 0 N = 3
0 = 1.0 M= 0.3 b= 0.05 H0 = 70 ns = 1.0 m = 3eV N = 3
0 = 1.0 M= 0.3 b= 0.05 H0 = 70 ns = 1.0 m = 3eV N = 8
0 = 1.0 M= 0.35 b= 0.05 H0 = 70 ns = 1.0 m = 3eV N = 8
STH, JCAP 0305, 004 (2003), STH & G RAFFELT JCAP 0404, 008 (2004)
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THE UPPER MASS LIMIT ON EACH INDIVIDUAL MASS EIGENSTATEIS ROUGHLY CONSTANT FOR ALL N IF ALL SPECIES CARRY EQUALMASS
STH & G RAFFELT (JCAP 0404, 008 (2004))SEE ALSO CROTTY, LESGOURGUES & PASTOR HEP-PH/0402049
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Maltoni, Schweitz, Tortola & Valle ’03 (hep-ph/0305312)ONLY IF LYMAN-ALPHA AND BIAS CONSTRAINTS ARE INCLUDED ISTHE LSND SOLUTION EXCLUDED AT 95% C.L. (SELJAK ET AL. 2004)
A GLOBAL ANALYSIS STILL LEAVES THE TWO LOWEST LYING ISLANDSIN PARAMETER SPACE FOR LSND!
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WHAT ABOUT OTHER LIGHT, THERMALLYPRODUCED PARTICLES?
NEUTRINOS
AXIONS
GRAVITONS
MAJORONS
AXINOS
RADIONS
...........
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FOR ANY THERMALLY PRODUCED PARTICLE IT ISSTRAIGHTFORWARD TO CALCULATE THE DECOUPLINGEPOCH ETC.THE ONLY IMPORTANT PARAMETERS ARE
Xm
WHERE g* IS THE EFECTIVE NUMBER OF DEGREES OFFREEDOM WHEN X DECOUPLES.
*,XgAND
bosonsfor 3/4
fermionsfor 175.10
eV 183 *
2
X
XXX g
gmh
2
24
2X
FS 9.3log1Mpc 20
~Xm
XX
T
T
T
T
h
CONTRIBUTION TO DENSITY
FREE-STREAMING LENGTH
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EW transition (~ 100 GeV)g* = 106.75
Density bound for a Majorana fermion
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
Based on WMAP, SDSS, SNI-a and Lyman- data, No assumptions about bias!
MASS BOUND FOR SPECIES DECOUPLINGAROUND EW TRANSITION
eV 5m
DECOUPLING AFTERQCD PHASE TRANSITIONLEADS TO
eV 1m
Below QCD transition (~ 100 MeV) g* < 20
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NOTE THAT MASS BOUNDS CANNOT BE DIRECTLY EXTENDEDTO RELIC PARTICLES WHICH MAKE UP MORE THAN A SMALLFRACTION OF THE TOTAL DENSITY!!
LYMAN-ALPHA ANALYSIS IS BASED ON THE ASSUMPTION THATTHE POWER SPECTRUM IS CLOSE TO A POWER-LAW
IF THERE IS EXPONENTIAL DAMPING THEN THE ”RAW” LYMAN-ALPHA DATA SHOULD BE USED DIRECTLY AND COMPAREDWITH NUMERICAL SIMULATIONS
THIS HAS BEEN DONE BY VIEL ET AL. astro-ph/0501562
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VIEL ET AL. astro-ph/0501562
THE 2LOWER BOUND ON THE MASS OF THE WDM PARTICLE IS ~ 500 eV
THE BEST FIT IS NOT ATINFINITE MASS ALTHOUGHTHE EFFECT IS NOT STATISTICALLY SIGNIFICANT
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WHAT IS IN STORE FOR THE FUTURE?
LARGE SCALE STRUCTURE SURVEYS2dF (completed) 250.000 galaxies SDSS (ongoing) 1.000.000 galaxies
COSMOLOGICAL SUPERNOVA SURVEYSSNLS, DARK ENERGY CAMERA, SNAP
WEAK LENSING SURVEYS (Pan-STARRS 2006, LSST 2012)
BETTER CMBR TEMPERATURE MEASUREMENTS
Satellites Balloons InterferometersWMAP (ongoing) Boomerang (2002-2003) CBI (ongoing)Planck (2007) TopHat (ongoing) DASI (ongoing)
CMBR POLARIZATION MEASUREMENTS
Satellites Balloons GroundWMAP (ongoing) Boomerang (2002-3) Polatron (ongoing)Planck (2007) DASI
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CMB POLARIZATION ANISOTROPY MEASUREMENT
Tlm
Elm
ETl aaC *
),(),(),( ,, Bablm
Blm
lm
Eablm
Elm
ab YaYaT
P
Gives a new sequence ofpower spectra
Elm
Elm
EEl aaC *
Blm
Blm
BBl aaC *
Dodelson & Hu ’01
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PROJECTED OBSERVATIONAL ERRORS FOR MAP AND PLANCK
WMAP FINAL DATA (4 YEARS) PLANCK (STARTING 2007)
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SNAP SATELLITE
http://snap.lbl.gov
THE SUPERNOVAACCELERATIONPROBE (SNAP) WILLOBSERVE ROUGHLY2000 TYPEI-a SN OUTTO REDSHIFTS OFORDER 1.5, STARTINGFROM ~ 2012?
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Distortion of background images by foreground matter
Unlensed Lensed
WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE
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H
drPa
gHC m
0
2
240 ),/(
)(
16
9
H
dng
0
''
)'()'(2)(
FROM A WEAK LENSING SURVEY THE ANGULAR POWER SPECTRUMCAN BE CONSTRUCTED, JUST LIKE IN THE CASE OF CMB
),/( rP MATTER POWER SPECTRUM (NON-LINEAR)
WEIGHT FUNCTION DESCRIBING LENSINGPROBABILITY
(SEE FOR INSTANCE JAIN & SELJAK ’96, ABAZAJIAN & DODELSON ’03,SIMPSON & BRIDLE ’04)
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Non-linear physics
Wide survey
WEAK LENSING POWER SPECTRUM
FIRST PROJECT Pan-STARRS WILL START IN JANUARY 2006
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MASS BOUNDS ON LIGHT PARTICLESWILL IMPROVE SIGNIFICANTLY IN THE FUTURE, PERHAPS EVEN TO 0.1 eVFOR THE SUM OF NEUTRINO MASSES