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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Geheimnis der dunklen MaterieGeheimnis der dunklen Materie
Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen
Topical Seminar Neutrino Physics & Astrophysics1721 Sept 2008, Beijing, China
Topical Seminar Neutrino Physics & Astrophysics1721 Sept 2008, Beijing, China
The Dark Universe, Neutrinos,The Dark Universe, Neutrinos,and Cosmological Mass Boundsand Cosmological Mass Bounds
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
ThomasThomas WrightWright (1750),(1750), AnAn OriginalOriginal TheoryTheory ofof
thethe UniverseUniverse
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
TitleTitle
Dark Energy 73%Dark Energy 73%(Cosmological Constant)(Cosmological Constant)
NeutrinosNeutrinos 0.10.12%2%
Dark MatterDark Matter23%23%
Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about 10% luminous)10% luminous)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Coma ClusterComa Cluster
Dark Matter in Galaxy ClustersDark Matter in Galaxy Clusters
A gravitationally boundA gravitationally boundsystem of many particlessystem of many particlesobeys the virial theoremobeys the virial theorem
gravkin EE2 gravkin EE2
rmMG
2mv
2 rN2
r
mMG2
mv2 rN
2
1rN
2 rMGv 1rN
2 rMGv
Velocity dispersionVelocity dispersionfrom Doppler shiftsfrom Doppler shiftsand geometric sizeand geometric size
Total MassTotal Mass
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Dark Matter in Galaxy ClustersDark Matter in Galaxy Clusters
Fritz Zwicky:Fritz Zwicky:Die Rotverschiebung von Die Rotverschiebung von Extragalaktischen NebelnExtragalaktischen Nebeln(The redshift of extragalactic(The redshift of extragalactic nebulae)nebulae)Helv. Phys. Acta 6 (1933) 110Helv. Phys. Acta 6 (1933) 110
In order to obtain the observed average Doppler effect ofIn order to obtain the observed average Doppler effect of1000 km/s or more, the average density of the Coma cluster1000 km/s or more, the average density of the Coma clusterwould have to be at least 400 times larger than what is foundwould have to be at least 400 times larger than what is foundfrom observations of the luminous matter.from observations of the luminous matter.Should this be confirmed one would find the surprising resultShould this be confirmed one would find the surprising resultthat that dark matter dark matter is far more abundant than luminous matter.is far more abundant than luminous matter.
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure of Spiral GalaxiesStructure of Spiral Galaxies
Spiral Galaxy NGC 2997 Spiral Galaxy NGC 891891
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Rotation curve of the galaxy NGC 6503Rotation curve of the galaxy NGC 6503from radio observations of hydrogen motionfrom radio observations of hydrogen motion[MNRAS 249 (1991) 523][MNRAS 249 (1991) 523]
Galactic Rotation Curve from Radio ObservationsGalactic Rotation Curve from Radio Observations
Expected from Expected from luminous matter in luminous matter in the diskthe disk
Observed Observed flat rotation flat rotation curvecurve
Spiral galaxy NGC 3198 overlaidSpiral galaxy NGC 3198 overlaidwith hydrogen column densitywith hydrogen column density[ApJ 295 (1985) 305][ApJ 295 (1985) 305]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure of a Spiral GalaxyStructure of a Spiral Galaxy
Dark HaloDark Halo
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Expanding Universe and the Big BangExpanding Universe and the Big Bang
Hubble’s lawHubble’s law
vvexpansionexpansion = H = H00
distancedistance Hubble’s constantHubble’s constant
HH00 = h 100 km s = h 100 km s-1-1 Mpc Mpc-1-1
Measured valueMeasured value
h = 0.72 h = 0.72 0.04 0.04
Expansion age of the universeExpansion age of the universe
tt00 H H0011 14 14 10 1099 years years
1 Mpc = 3.26 1 Mpc = 3.26 10 1066 lyrlyr
= 3.08 = 3.08 10 102424 cmcm
• PhotonsPhotons• NeutrinosNeutrinos• Charged LeptonsCharged Leptons• QuarksQuarks• GluonsGluons• W- and Z-Bosons W- and Z-Bosons • Higgs ParticlesHiggs Particles• GravitonsGravitons• Dark-Matter ParticlesDark-Matter Particles• Topological defectsTopological defects• … …
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Big BangBig Bang
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Cosmic ExpansionCosmic Expansion
• Space between galaxies growsSpace between galaxies grows• GalaxiesGalaxies (stars,(stars, people)people) stay the same stay the same (dominated by local gravity(dominated by local gravity or by electromagnetic forces)or by electromagnetic forces)• Cosmic scale factor today: Cosmic scale factor today: a = 1a = 1
Cosmic Scale FactorCosmic Scale Factor Cosmic RedshiftCosmic Redshift
• Wavelength of light gets “stretched”Wavelength of light gets “stretched”
• Suffers redshiftSuffers redshift
• Redshift today: Redshift today: z = 0z = 0
then
today1z
then
today1z
then
today
then
today
a
a1z
then
today
then
today
a
a1z
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Friedman Equation & Einstein’s “Greatest Friedman Equation & Einstein’s “Greatest Blunder”Blunder”
Friedmann equation forFriedmann equation for Hubble’s expansion rateHubble’s expansion rate 3a
k3
NG8
aa
H2
22
3a
k3
NG8
aa
H2
22
YakovYakovBorisovichBorisovichZeldovichZeldovich1914-19871914-1987
• Quantum field theory of elementary particlesQuantum field theory of elementary particles inevitably implies vacuum fluctuations becauseinevitably implies vacuum fluctuations because of Heisenberg’s uncertainty relation,of Heisenberg’s uncertainty relation, e.g. E and B fields can not simultaneously vanish e.g. E and B fields can not simultaneously vanish • Ground state (vacuum) provides gravitating energyGround state (vacuum) provides gravitating energy
• Vacuum energy Vacuum energy vacvac is equivalent to is equivalent to
Cosmological constant (new constant of nature)allows for a static universeby “global anti-gravitation”
Newton’s constantNewton’s constant
Density of gravitating mass & energyDensity of gravitating mass & energy Curvature termCurvature termis very small or zerois very small or zero(Euclidean spatial geometry)(Euclidean spatial geometry)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Generic Solutions of Friedmann EquationGeneric Solutions of Friedmann Equation
RadiationRadiation p = p = /3/3 aa44 a(t) a(t) tt1/21/2 Dilution of radiationDilution of radiationand redshift of energyand redshift of energy
MatterMatter p = 0p = 0 aa33 a(t) a(t) tt2/32/3Dilution of matterDilution of matter
VacuumVacuumenergyenergy p = p = = const= const Vacuum energy notVacuum energy not
diluted by expansiondiluted by expansion
t3exp)t(a t3exp)t(a
vacNG8 vacNG8
EquationEquationof stateof state
Behavior of energy-density underBehavior of energy-density undercosmic expansioncosmic expansion
Evolution ofEvolution ofcosmic scale factorcosmic scale factor
Energy-momentum tensor of perfect fluid with density Energy-momentum tensor of perfect fluid with density and pressure p and pressure p
p
p
pT
p
p
pT
gTvac
gTvac
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Hubble DiagramHubble Diagram
Supernova IaSupernova Ia as cosmologicalas cosmological standard candlesstandard candles
RedshiftRedshift
Ap
pare
nt
Bri
gh
tness
Ap
pare
nt
Bri
gh
tness
Hubble’s orginal data (1929)Hubble’s orginal data (1929)
zz == 0.0030.003
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Hubble DiagramHubble Diagram
Accelerated expansionAccelerated expansion((MM == 0.3, 0.3, == 0.7)0.7)
Decelerated expansionDecelerated expansion((MM == 1)1)
Supernova IaSupernova Ia as cosmologicalas cosmological standard candlesstandard candles
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Latest Supernova DataLatest Supernova Data
Kowalski et al.,Kowalski et al.,Improved cosmological constraints from new, old andImproved cosmological constraints from new, old andcombined supernova datasets, arXiv:0804.4142combined supernova datasets, arXiv:0804.4142
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Expansion of Different Cosmological ModelsExpansion of Different Cosmological Models
Time (billion years)Time (billion years)
Adapted from Bruno Leibundgut
Cosmic scale Cosmic scale factor afactor a
todaytoday1414
MM = 0 = 0
99
MM = 1 = 1
77
MM > 1 > 1
MM = 0.3 = 0.3
= 0.7= 0.7
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
TitleTitle
Dark Energy 73%Dark Energy 73%(Cosmological Constant)(Cosmological Constant)
NeutrinosNeutrinos 0.10.12%2%
Dark MatterDark Matter23%23%
Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about 10% luminous)10% luminous)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrino Thermal EquilibriumNeutrino Thermal Equilibrium
Cosmic expansion rateCosmic expansion rate
Friedmann equationFriedmann equation
2Plm
238
H 2
Plm2
38
H
4T~ 4T~
Pl
2
mT~HPl
2
mT~H
Radiation dominatesRadiation dominates
Expansion rateExpansion rate
Condition for thermal equilibrium: Condition for thermal equilibrium: > H > H
MeV1])GeV10(GeV10[~)Gm(T 3122519312FPl MeV1])GeV10(GeV10[~)Gm(T 3122519312FPl
Neutrinos are in thermal equilibrium for T Neutrinos are in thermal equilibrium for T ≳ 1 MeV≳ 1 MeVcorresponding to t ≲ 1 seccorresponding to t ≲ 1 sec
ee ee
Neutrino reactionsNeutrino reactions
Dimensional analysis of reaction rateDimensional analysis of reaction rateif T if T ≪≪ m mW,ZW,Z
52FTG~ 52FTG~
Examples for neutrino processesExamples for neutrino processes
ee ee
GGFF
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Present-Day Neutrino DensityPresent-Day Neutrino Density
Neutrino decouplingNeutrino decoupling(freeze out)(freeze out)
H ~ H ~ T T 2.4 MeV 2.4 MeV (electron flavor) (electron flavor) T T 3.7 MeV 3.7 MeV (other flavors) (other flavors)
Redshift of Fermi-DiracRedshift of Fermi-Diracdistribution (“nothingdistribution (“nothingchanges at freeze-out”)changes at freeze-out”)
1e
E1dE
dNT/E
2
2
1e
E1dE
dNT/E
2
2
TemperatureTemperaturescales with redshiftscales with redshiftTT = T = T (z+1) (z+1)
Electron-positronElectron-positronannihilation beginning annihilation beginning
at T at T m mee = 0.511 MeV = 0.511 MeV
• QED plasma is “strongly” coupledQED plasma is “strongly” coupled• Stays in thermal equilibrium (adiabatic process)Stays in thermal equilibrium (adiabatic process)• Entropy of eEntropy of e++ee transfered to photons transfered to photons
after3
before3 TgTg
after3
before3 TgTg
42 8
742 8
722 before
3114
after3 TT
before3
114
after3 TT
Redshift ofRedshift ofneutrino and photonneutrino and photonthermal distributionsthermal distributionsso that today we haveso that today we have
3113
43
114 cm112nn)flavor1(n
3113
43
114 cm112nn)flavor1(n
K95.1T114
T31
K95.1T114
T31
for massless neutrinosfor massless neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses
A classic paper:A classic paper: Gershtein & ZeldovichGershtein & Zeldovich JETP Lett. 4 (1966) 120JETP Lett. 4 (1966) 120
4.0eV5.92
mh2
4.0eV5.92
mh2
Cosmic neutrino “sea”Cosmic neutrino “sea” ~ 112 cm~ 112 cm-3-3 neutrinos + anti-neutrinos per neutrinos + anti-neutrinos per flavorflavor
mm ≲≲ 40 eV 40 eV For allFor allstable flavorsstable flavors
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Weakly Interacting Particles as Dark MatterWeakly Interacting Particles as Dark Matter
However, the idea ofHowever, the idea of weakly interacting massiveweakly interacting massive particles as dark matterparticles as dark matter is now standardis now standard
• More than 30 years ago,More than 30 years ago, beginnings of the idea ofbeginnings of the idea of weakly interacting particlesweakly interacting particles (neutrinos) as dark matter(neutrinos) as dark matter
• Massive neutrinos are noMassive neutrinos are no longer a good candidatelonger a good candidate (hot dark matter)(hot dark matter)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
What is wrong with neutrino dark matter?What is wrong with neutrino dark matter?
Galactic Phase Space (“Tremaine-Gunn-Limit”)Galactic Phase Space (“Tremaine-Gunn-Limit”)
mm >> 20 20 40 eV 40 eV
2
3escape
n
2
3max
max3
)vm(m
3
pm
max
2
3escape
n
2
3max
max3
)vm(m
3
pm
max
Maximum mass density of a degenerateMaximum mass density of a degenerateFermi gasFermi gas
mm >> 100 100 200 eV 200 eV
SpiralSpiral galaxiesgalaxies
DwarfDwarf galaxiesgalaxies
• Nus are “Hot Dark Matter”Nus are “Hot Dark Matter”• Ruled out Ruled out by structure formationby structure formation
Neutrino Free Streaming (Collisionless Phase Mixing)Neutrino Free Streaming (Collisionless Phase Mixing)
• AtAt TT << 11 MeVMeV neutrinoneutrino scatteringscattering inin earlyearly universeuniverse ineffectiveineffective• Stream freely until non-relativisticStream freely until non-relativistic• Wash out density contrasts on small scales Wash out density contrasts on small scales
NeutrinosNeutrinosNeutrinosNeutrinos
Over-densityOver-density
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Sky Distribution of Galaxies (XMASS XSC)Sky Distribution of Galaxies (XMASS XSC)
http://spider.ipac.caltech.edu/staff/jarrett/2mass/XSC/jarrett_allsky.html
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
A Slice of the UniverseA Slice of the Universe
Galaxy distribution from the CfA redshift surveyGalaxy distribution from the CfA redshift survey[ApJ 302 (1986) L1][ApJ 302 (1986) L1]
Cosmic Cosmic ““Stick Man”Stick Man”
~ 185 Mpc
~ 185 Mpc
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
2dF Galaxy Redshift Survey (2002)2dF Galaxy Redshift Survey (2002)
~ 1300 M
pc
~ 1300 M
pc
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
SDSS SurveySDSS Survey
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Generating the Primordial Density FluctuationsGenerating the Primordial Density Fluctuations
Zero-point fluctuations of quantumZero-point fluctuations of quantumfields are stretched and frozenfields are stretched and frozen
Early phase of exponential expansionEarly phase of exponential expansion(Inflationary epoch)(Inflationary epoch)
Cosmic density fluctuations areCosmic density fluctuations arefrozen quantum fluctuationsfrozen quantum fluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Gravitational Growth of Density PerturbationsGravitational Growth of Density Perturbations
The dynamical evolutionThe dynamical evolutionof small perturbationsof small perturbations
1)x(
)x(
1
)x()x(
is independent for eachis independent for eachFourier mode Fourier mode kk
• For pressureless,For pressureless, nonrelativistic matternonrelativistic matter (cold dark matter)(cold dark matter) naively expectnaively expect exponential growthexponential growth
• Only power-lawOnly power-law growth in expandinggrowth in expanding universeuniverse
Matter dominatesMatter dominates a a tt2/32/3
Sub-horizonSub-horizon ≪≪ HH11
Super-horizonSuper-horizon ≫≫ HH11
kk const const kk a a22 tt
kk a a tt2/32/3
Radiation dominatesRadiation dominates a a tt1/21/2
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure Formation by Gravitational Structure Formation by Gravitational InstabilityInstability
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Redshift Surveys vs. Millenium SimulationRedshift Surveys vs. Millenium Simulation
www.mpa-garching.mpg.de/millennium
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Power Spectrum of Density FluctuationsPower Spectrum of Density Fluctuations
Field of density fluctuationsField of density fluctuations
)x(
)x(
)x()x(
Fourier transformFourier transform
)x(exd xik3k )x(exd xik3k
Power spectrum essentially squarePower spectrum essentially squareof Fourier transformationof Fourier transformation
)k(Pkkˆ2 3kk )k(Pkkˆ2 3kk
Power spectrum is Fourier transform ofPower spectrum is Fourier transform oftwo-point correlation function (two-point correlation function (x=xx=x22xx11) )
)k(Pe
2
kd)x()x()x( xik
3
3
12
)k(Pe
2
kd)x()x()x( xik
3
3
12
)k(
2
3xik
2
2
)k(Pke
kdk
4d
)k(
2
3xik
2
2
)k(Pke
kdk
4d
with the with the -function-function
Gaussian random field (phases ofGaussian random field (phases ofFourier modes Fourier modes kk uncorrelated) is fully uncorrelated) is fully
characterized by the power spectrumcharacterized by the power spectrum2
k)k(P 2k)k(P
or equivalently byor equivalently by
2k
2
)k(Pk)k( k
2321
2
3
2k
2
)k(Pk)k( k
2321
2
3
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Processed Power Spectrum in Cold Dark Matter Processed Power Spectrum in Cold Dark Matter ScenarioScenario
Primordial spectrumPrimordial spectrumusually assumed to beusually assumed to beof power-law formof power-law form
n2k k)k(P n2k k)k(P
Harrison-ZeldovichHarrison-Zeldovich(“flat”) spectrum(“flat”) spectrum n n 1 1expected from inflationexpected from inflation(actually slightly less(actually slightly less than 1, as confirmedthan 1, as confirmed by precision data)by precision data)
PrimordialPrimordialspectrumspectrum
Suppressed by stagnationSuppressed by stagnationduring radiation phaseduring radiation phase
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Power Spectrum of Cosmic Density Power Spectrum of Cosmic Density FluctuationsFluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Cosmic Microwave Background RadiationCosmic Microwave Background Radiation
Discovery of 2.7 KelvinDiscovery of 2.7 KelvinCosmic microwave background radiationCosmic microwave background radiationby Penzias and Wilson in 1965by Penzias and Wilson in 1965(Nobel Prize 1978)(Nobel Prize 1978)
Beginning of “big-bang cosmology”Beginning of “big-bang cosmology”
Robert W. WilsonRobert W. WilsonBorn 1936Born 1936
Arno A. Penzias Arno A. Penzias Born 1933Born 1933
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Last Scattering SurfaceLast Scattering Surface
1133
202010
00
1000
1500
1500
Redshift zRedshift z
Here & Here & NowNow
HorizonHorizon
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
COBE Temperature Map of the Cosmic Microwave COBE Temperature Map of the Cosmic Microwave BackgroundBackground
T = 2.725 K (uniform on the sky)T = 2.725 K (uniform on the sky)Dynamical range Dynamical range T = 3.353 mK (T = 3.353 mK (T/T/ T T 10 10-3-3))
Dipole temperature distribution from Doppler effectDipole temperature distribution from Doppler effectcaused by our motion relative to the cosmic framecaused by our motion relative to the cosmic frame
Dynamical range Dynamical range T = 18 T = 18 K (K (T/T/ T T 10 10-5-5))
Primordial temperature fluctuationsPrimordial temperature fluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
COBE SatelliteCOBE Satellite
John C. Mather John C. Mather Born 1946Born 1946
George F. Smoot George F. Smoot Born 1945Born 1945
Nobel Prize 2006Nobel Prize 2006
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Sky map of CMBR temperatureSky map of CMBR temperaturefluctuationsfluctuations
T
T,T,
TT,T
,
Power Spectrum of CMBR Temperature Power Spectrum of CMBR Temperature FluctuationsFluctuations
Multipole expansionMultipole expansion
,Ya, m
0 mm
,Ya, m
0 mm
Angular power spectrumAngular power spectrum
mmmmm aa
121
aaC
mmmmm aa
121
aaC
Acoustic PeaksAcoustic Peaks
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Flat Universe from CMBR Angular FluctuationsFlat Universe from CMBR Angular Fluctuations
totmax 200 totmax 200
tot tot = 1.02 = 1.02 0.02 0.02
Spergel et al. (WMAP Collaboration)Spergel et al. (WMAP Collaboration)astro-ph/0302209astro-ph/0302209
Triangulation with acoustic peakTriangulation with acoustic peak
Known physicalKnown physical size of acoustic peaksize of acoustic peak at decoupling (zat decoupling (z 1100)1100)
MeasuredMeasuredangular sizeangular sizetoday (ztoday (z == 0)0)
flat (Euclidean)flat (Euclidean)
negative curvaturenegative curvature
positive curvaturepositive curvature
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Latest CMB Results (WMAP-5 and Others)Latest CMB Results (WMAP-5 and Others)
Komatsu et al., arXiv:0803.0547Komatsu et al., arXiv:0803.0547
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Best-Fit UniverseBest-Fit Universe
PerlmutterPhysics Today(Apr. 2003)
Kowalski et al.arXiv:0804.4142
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Concordance Model of CosmologyConcordance Model of Cosmology
A Friedmann-Lemaître-Robertson-Walker model with the followingA Friedmann-Lemaître-Robertson-Walker model with the followingparameters perfectly describes the global properties of the universe parameters perfectly describes the global properties of the universe
The observed large-scale structure and CMBR temperature fluctuationsThe observed large-scale structure and CMBR temperature fluctuationsare perfectly accounted for by the gravitational instability mechanismare perfectly accounted for by the gravitational instability mechanismwith the above ingredients and a power-law primordial spectrum of with the above ingredients and a power-law primordial spectrum of adiabatic density fluctuations (curvature fluctuations) P(k) adiabatic density fluctuations (curvature fluctuations) P(k) k knn
Expansion rateExpansion rate 110 Mpcskm)3.11.70(H 110 Mpcskm)3.11.70(H
AgeAge years10)12.073.13(t 90 years10)12.073.13(t 90
Vacuum energyVacuum energy 015.0721.0 015.0721.0
Baryonic matterBaryonic matter 0015.00462.0B 0015.00462.0B
Power-law indexPower-law index 014.0960.0n 014.0960.0n
Spatial curvatureSpatial curvature Gpc33Rcurv Gpc33Rcurv 009.0018.0 k 009.0018.0 k
Cold Dark MatterCold Dark Matter 013.0233.0CDM 013.0233.0CDM
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure Formation in the UniverseStructure Formation in the Universe
SmoothSmooth StructuredStructured
Structure forms byStructure forms by gravitational instabilitygravitational instability of primordialof primordial density fluctuationsdensity fluctuations
A fraction of hot dark matter A fraction of hot dark matter suppresses small-scale structuresuppresses small-scale structure
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure Formation with Hot Dark MatterStructure Formation with Hot Dark Matter
Troels Haugbølle, http://whome.phys.au.dk/~haugboelTroels Haugbølle, http://whome.phys.au.dk/~haugboel
Neutrinos with Neutrinos with mm = 6.9 eV = 6.9 eVStandard Standard CDM ModelCDM Model
Structure fromation simulated with Gadget codeStructure fromation simulated with Gadget codeCube size 256 Mpc at zero redshiftCube size 256 Mpc at zero redshift
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrino Free Streaming: Transfer FunctionNeutrino Free Streaming: Transfer Function
Hannestad, Neutrinos in Cosmology, hep-ph/0404239Hannestad, Neutrinos in Cosmology, hep-ph/0404239
Transfer functionTransfer function
P(k) = T(k) PP(k) = T(k) P00(k)(k)
Effect of neutrino freeEffect of neutrino freestreaming on small scalesstreaming on small scales
T(k) = 1 T(k) = 1 8 8//M M
valid forvalid for
88//M M ≪ ≪ 11
Power suppression for Power suppression for FSFS ≳ ≳ 100 Mpc/h100 Mpc/h
mm = 0 = 0
mm = 0.3 eV = 0.3 eV
mm = 1 eV = 1 eV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Power Spectrum of Cosmic Density Power Spectrum of Cosmic Density FluctuationsFluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Some Recent Cosmological Limits on Neutrino Some Recent Cosmological Limits on Neutrino MassesMassesmm/eV/eV(limit 95%CL)(limit 95%CL)
Data / PriorsData / Priors
Spergel et al. (WMAP) 2003Spergel et al. (WMAP) 2003 [astro-ph/0302209] [astro-ph/0302209] 0.690.69 WMAP-1, 2dF, HST, WMAP-1, 2dF, HST, 88
Hannestad 2003Hannestad 2003 [astro-ph/0303076][astro-ph/0303076]1.011.01 WMAP-1, CMB, 2dF, HSTWMAP-1, CMB, 2dF, HST
Crotty et al. 2004Crotty et al. 2004 [hep-ph/0402049][hep-ph/0402049]
1.01.00.60.6
WMAP-1, CMB, 2dF, SDSSWMAP-1, CMB, 2dF, SDSS& HST, SN& HST, SN
Hannestad 2004Hannestad 2004 [hep-ph/0409108][hep-ph/0409108] 0.650.65 WMAP-1, SDSS, SN Ia gold sample,WMAP-1, SDSS, SN Ia gold sample,
Ly-Ly- data from Keck sample data from Keck sample
Seljak et al. 2004Seljak et al. 2004 [[astro-ph/0407372]astro-ph/0407372]0.420.42 WMAP-1, SDSS, Bias,WMAP-1, SDSS, Bias,
Ly-Ly- data from SDSS sample data from SDSS sample
Spergel et al. 2006Spergel et al. 2006 [hep-ph/0409108][hep-ph/0409108] 0.680.68 WMAP-3, SDSS, 2dF, SN Ia, WMAP-3, SDSS, 2dF, SN Ia, 88
Seljak et al. 2006Seljak et al. 2006 [astro-ph/0604335][astro-ph/0604335]0.140.14 WMAP-3, CMB-small, SDSS, 2dF,WMAP-3, CMB-small, SDSS, 2dF,
SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), Ly-Ly- (SDSS) (SDSS)
Hannestad et al. 2006Hannestad et al. 2006 [hep-ph/0409108][hep-ph/0409108] 0.300.30 WMAP-1, CMB-small, SDSS, 2dF,WMAP-1, CMB-small, SDSS, 2dF,
SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), Ly-Ly- (SDSS) (SDSS)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Lyman-alpha ForestLyman-alpha Forest
• Hydrogen clouds absorb from QSOHydrogen clouds absorb from QSO continuum emission spectrumcontinuum emission spectrum
• Absorption dips at Ly-Absorption dips at Ly- wavelengh wavelengh corresponding to redshiftcorresponding to redshift
www.astro.ucla.edu/~wright/Lyman-alpha-forest.htmlwww.astro.ucla.edu/~wright/Lyman-alpha-forest.html
Examples for Lyman-Examples for Lyman- forest in forest inlow- and high-redshift quasarslow- and high-redshift quasars
http://www.astr.ua.edu/keel/agn/forest.gifhttp://www.astr.ua.edu/keel/agn/forest.gif
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Weak Lensing Weak Lensing A Powerful Probe for the Future A Powerful Probe for the Future
UnlensedUnlensed LensedLensed
Distortion of background images by foreground matterDistortion of background images by foreground matter
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Sensitivity Forecasts for Future LSS Sensitivity Forecasts for Future LSS ObservationsObservations
Kaplinghat, Knox & Song,Kaplinghat, Knox & Song,astro-ph/0303344astro-ph/0303344
σσ(m(mνν) ~ 0.15 eV ) ~ 0.15 eV (Planck)(Planck)
σσ(m(mνν) ~ 0.044 eV (CMBpol)) ~ 0.044 eV (CMBpol)CMB lensing CMB lensing
Lesgourgues, PastorLesgourgues, Pastor& Perotto,& Perotto,hep-ph/0403296 hep-ph/0403296
Planck & SDSS Planck & SDSS mm > 0.21 eV detectable > 0.21 eV detectable
at 2at 2
mm > 0.13 eV detectable > 0.13 eV detectable
at 2at 2Ideal CMB & 40 x SDSS Ideal CMB & 40 x SDSS
Abazajian & DodelsonAbazajian & Dodelsonastro-ph/0212216astro-ph/0212216
Future weak lensingFuture weak lensingsurvey 4000 degsurvey 4000 deg22
σσ(m(mνν) ~ 0.1 eV) ~ 0.1 eV
Wang, Haiman, Hu, Wang, Haiman, Hu, Khoury & May,Khoury & May,astro-ph/0505390astro-ph/0505390
Weak-lensing selectedWeak-lensing selectedsample of > 10sample of > 105 5 clustersclusters
σσ(m(mνν) ~ 0.03 eV) ~ 0.03 eV
Hannestad, Tu & WongHannestad, Tu & Wongastro-ph/0603019astro-ph/0603019
Weak-lensing tomographyWeak-lensing tomography(LSST plus Planck)(LSST plus Planck) σσ(m(mνν) ~ 0.05 eV) ~ 0.05 eV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Fermion Mass SpectrumFermion Mass Spectrum
1010 10010011 1010 10010011 1010 10010011 1010 10010011 1010 10010011 11meVmeV eVeV keVkeV MeVMeV GeVGeV TeVTeV
dd ss bbQuarks (Q = Quarks (Q = 1/3)1/3)
uu cc ttQuarks (Q = Quarks (Q = 2/3)2/3)
Charged Leptons (Q = Charged Leptons (Q = 1)1) ee
All flavorsAll flavors
33 NeutrinosNeutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
““Weighing” Neutrinos with KATRINWeighing” Neutrinos with KATRIN
• Sensitive to Sensitive to common mass scale mcommon mass scale m for all flavors because of small massfor all flavors because of small mass differences from oscillationsdifferences from oscillations• Best limit from Mainz und TroitskBest limit from Mainz und Troitsk m m << 2.2 eV (95% CL) 2.2 eV (95% CL)• KATRIN can reach KATRIN can reach 0.2 eV0.2 eV• Under constructionUnder construction• Data taking foreseen to begin in 2009Data taking foreseen to begin in 2009
http://www-ik.fzk.de/katrin/http://www-ik.fzk.de/katrin/
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
““KATRIN Approaching” (25 Nov 2006)KATRIN Approaching” (25 Nov 2006)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Lee-Weinberg Curve for Neutrinos and AxionsLee-Weinberg Curve for Neutrinos and Axions
log(log(aa))
log(mlog(maa))
MM
10 eV10 eV 10 10 eVeV
CDCDMM
HDHDMMAxionsAxions
Thermal RelicsThermal RelicsNon-ThermalNon-Thermal
RelicsRelics
log(log())
log(mlog(m))
MM
10 eV10 eV
CDCDMM
HDHDMM
10 GeV10 GeV
NeutrinosNeutrinos& WIMPs& WIMPs
Thermal RelicsThermal Relics
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Axion Hot Dark Matter from Thermalization Axion Hot Dark Matter from Thermalization after after QCDQCD
Freeze-out temperatureFreeze-out temperature
Cosmic thermal degrees ofCosmic thermal degrees offreedom at axion freeze-outfreedom at axion freeze-out
Cosmic thermal degrees ofCosmic thermal degrees offreedom freedom
a)2
(ff
CL
0
00
a
aa
a)2
(ff
CL
0
00
a
aa
aa
Chang & Choi, PLB 316 (1993) 51Chang & Choi, PLB 316 (1993) 51Hannestad, Mirizzi & Raffelt, JCAP 07 (2005) 02Hannestad, Mirizzi & Raffelt, JCAP 07 (2005) 02
094.0)z1(3
z1Ca
094.0)z1(3
z1Ca
104 105 106 107
104 105 106 107
fa (GeV)
fa (GeV)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Low-Mass Particle Densities in the UniverseLow-Mass Particle Densities in the Universe
PhotonsPhotons
NeutrinosNeutrinos
Axions (QCD)Axions (QCD)
ALPsALPs(two photon vertex)(two photon vertex)
410 cm410 cm33Cosmic microwave backgroundCosmic microwave backgroundradiation radiation T = 2.725 KT = 2.725 K
Freeze out at Freeze out at T ~ 2T ~ 23 MeV3 MeVbefore ebefore eee annihilation annihilation
nn 113 nn 113
112 cm112 cm33 ( in one flavor)( in one flavor)
For fFor faa ~ 10 ~ 1077 GeV (m GeV (maa ~ 1 eV) ~ 1 eV)
Freeze out at Freeze out at T ~ 80 MeVT ~ 80 MeV((a interaction)a interaction)
~ 50 cm~ 50 cm33
Primakoff freeze outPrimakoff freeze out
(g(gaa ~ 10 ~ 101010 GeV GeV11))
T T ≫≫ T TQCDQCD ~ 200 MeV ~ 200 MeV< 10 cm< 10 cm33
• No useful hot dark matter limit on ALPs in the CAST search rangeNo useful hot dark matter limit on ALPs in the CAST search range (too few of them today if they couple only by two-photon vertex)(too few of them today if they couple only by two-photon vertex)
• Axion mass limit comparable to limit on Axion mass limit comparable to limit on mm
(Axion number density comparable to one neutrino flavor)(Axion number density comparable to one neutrino flavor)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Axion Hot Dark Matter Limits from Precision Axion Hot Dark Matter Limits from Precision DataData
mmaa < 1.0 eV (95% CL) < 1.0 eV (95% CL)
mmaa < 0.4 eV (95% CL) < 0.4 eV (95% CL)
WMAP-5, LSS, BAO, SNIaWMAP-5, LSS, BAO, SNIa
WMAP-3, small-scale CMB,WMAP-3, small-scale CMB,HST, BBN, LSS, HST, BBN, LSS, Ly-Ly-
Hannestad, Mirizzi, RaffeltHannestad, Mirizzi, Raffelt& Wong [arXiv:0803.1585]& Wong [arXiv:0803.1585]
Melchiorri, Mena & SlosarMelchiorri, Mena & Slosar[arXiv:0705.2695] [arXiv:0705.2695]
Marginalizing over unknown neutrino hot dark matter componentMarginalizing over unknown neutrino hot dark matter component
Credible regions for neutrino plus axion hotCredible regions for neutrino plus axion hotdark matter (WMAP-5, LSS, BAO, SNIa)dark matter (WMAP-5, LSS, BAO, SNIa)Hannestad, Mirizzi, Raffelt & WongHannestad, Mirizzi, Raffelt & Wong[arXiv:0803.1585][arXiv:0803.1585]
Dashed (red) curves: Same with WMAP-3Dashed (red) curves: Same with WMAP-3From HMRW [arXiv:0706.4198] From HMRW [arXiv:0706.4198]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
DirectDirectsearchsearch
Too muchToo muchcold dark mattercold dark matter
TeleTelescopescopeExperimentsExperiments
Globular clustersGlobular clusters(a-(a--coupling)-coupling)
Too manyToo manyeventsevents
Too muchToo muchenergy lossenergy loss
SN 1987A (a-N-coupling)SN 1987A (a-N-coupling)
Axion BoundsAxion Bounds
101033 101066 101099 10101212 [GeV] f[GeV] faa
eVeVkeVkeV meVmeV eVeVmmaa
Too much hot dark matterToo much hot dark matter
CASTCAST ADMXADMX
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
TitleTitle
Inner space andInner space andouter spaceouter space
are closely relatedare closely related