Cosmology and the Dark Universe · Quarks Leptons Charge +2/3 Up Charge −1/3 Down ... Neutrino...

Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City

Geheimnis der dunklen MaterieGeheimnis der dunklen Materie

Cosmology and theDark Universe

Cosmology and theDark Universe

Georg Raffelt, Max-Planck-Institut für Physik, MünchenGeorg Raffelt, Max-Planck-Institut für Physik, München

Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, MexicoEscuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico


Concordance Model of CosmologyConcordance Model of Cosmology

A FriedmannA Friedmann--LemaîtreLemaître--RobertsonRobertson--Walker model with the followingWalker model with the followingparameters perfectly describes the global properties of the univparameters perfectly describes the global properties of the universe erse

The observed largeThe observed large--scale structure and CMBR temperature fluctuationsscale structure and CMBR temperature fluctuationsare perfectly accounted for by the gravitational instability mecare perfectly accounted for by the gravitational instability mechanismhanismwith the above ingredients and a powerwith the above ingredients and a power--law primordial spectrum of law primordial spectrum of adiabatic density fluctuations (curvature fluctuations) P(k) adiabatic density fluctuations (curvature fluctuations) P(k) ∝∝ kknn

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 ±=ΛΩ 015.0721.0 ±=ΛΩ

Baryonic matterBaryonic matter 0015.00462.0B ±=Ω 0015.00462.0B ±=Ω

PowerPower--law indexlaw index 014.0960.0n ±= 014.0960.0n ±=

Spatial curvatureSpatial curvature Gpc33Rcurv > Gpc33Rcurv > 009.0018.0 k <<− Ω 009.0018.0 k <<− Ω

Cold Dark MatterCold Dark Matter 013.0233.0CDM ±=Ω 013.0233.0CDM ±=Ω


TitleTitle

Dark Energy 73%Dark Energy 73%(Cosmological Constant)(Cosmological Constant)

NeutrinosNeutrinos0.10.1−−2%2%

Dark MatterDark Matter23%23%

Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about10% luminous)10% luminous)


Expansion of Different Cosmological ModelsExpansion of Different Cosmological Models

Time (billion years)Time (billion years)

Adapted from Bruno Leibundgut

Cosmic scale factor aCosmic scale factor a

todaytoday−−1414

ΩΩMM = 0= 0

−−99

ΩΩMM = 1= 1

ΩΩMM = 0.3= 0.3ΩΩΛΛ = 0.7= 0.7


Dark Matter vs. Dark EnergyDark Matter vs. Dark Energy

Dark MatterDark Matter Dark EnergyDark Energy

Acts graviationally like ordinaryActs graviationally like ordinarymatter (attractive force)matter (attractive force)

•• Provides “negative pressure”Provides “negative pressure”•• “Anti“Anti--gravitation of the universe”gravitation of the universe”

Probably new form of weaklyProbably new form of weaklyinteracting particlesinteracting particles

•• Cosmological constant (classical GR)?Cosmological constant (classical GR)?•• Vacuum energy of quantum fields?Vacuum energy of quantum fields?•• Quintessence (new scalar field)?Quintessence (new scalar field)?

Dominates dynamics ofDominates dynamics ofgalaxies, clusters, larger structuresgalaxies, clusters, larger structures

Plays no role on small scalesPlays no role on small scales(homogeneous, does not cluster)(homogeneous, does not cluster)

Decelerates cosmic expansionDecelerates cosmic expansion Accelerates cosmic expansionAccelerates cosmic expansion

Possibly just an experimental problemPossibly just an experimental problem(detect the dark matter particles!)(detect the dark matter particles!)

Probably a fundamentalProbably a fundamentaltheory problemtheory problem


Periodic System of Elementary ParticlesPeriodic System of Elementary Particles

QuarksQuarks LeptonsLeptons

Charge +2/3 Charge +2/3

Up Up

Charge Charge −−1/3 1/3

Down Down

Charge Charge −−1 1

Electron Electron

Charge Charge 00

ee--Neutrino Neutrino ννeeeedduu

NeutronNeutron

ProtonProton





Up Up


Down Down


Electron Electron

Charge Charge 00

ee--Neutrino Neutrino ννeeeedduu

NeutronNeutron

ProtonProton



Up Up

Charm Charm

Top Top

Gravitation Gravitation

Weak InteractionWeak Interaction

Strong Interaction Strong Interaction

Electromagnetic InteractionElectromagnetic Interaction


Down Down

Strange Strange

Bottom Bottom


Electron Electron

Muon Muon

Tau Tau

Charge Charge 00

ee--Neutrino Neutrino

μμ--Neutrino Neutrino

ττ--Neutrino Neutrino ννττ

ννμμ

ννeeee

μμ

ττ

dd

ss

bb

uu

cc

tt

1. Family1. Family

2. Family 2. Family

3. Family3. Family



3. Neutrinos in Cosmology3. Neutrinos in Cosmology




Hans Bethe (1906Hans Bethe (1906−−2005, Nobel prize 1967)2005, Nobel prize 1967)Thermonuclear reaction chains (1938)Thermonuclear reaction chains (1938)

Neutrinos from the SunNeutrinos from the Sun

Solar radiation: 98 % lightSolar radiation: 98 % light2 % neutrinos2 % neutrinos

At Earth 66 billion neutrinos/cmAt Earth 66 billion neutrinos/cm22 secsec

ReactionReaction--chainschains

EnergyEnergy26.7 MeV26.7 MeV

HeliumHelium


Sun Glasses for Neutrinos?Sun Glasses for Neutrinos?

Several light years of lead Several light years of lead needed to shield solarneeded to shield solarneutrinosneutrinos

Bethe & Peierls 1934:Bethe & Peierls 1934:“… this evidently means“… this evidently meansthat one will never be ablethat one will never be ableto observe a neutrino.”to observe a neutrino.”

8.3 light minutes8.3 light minutes


First Detection (1954 First Detection (1954 -- 1956)1956)

Fred ReinesFred Reines(1918 (1918 –– 1998)1998)

Nobel prize 1995Nobel prize 1995

Clyde CowanClyde Cowan(1919 (1919 –– 1974)1974)

Detector prototypeDetector prototype

AntiAnti--Electron Electron NeutrinosNeutrinosfrom from Hanford Hanford Nuclear ReactorNuclear Reactor

3 Gammas3 Gammasin coincidencein coincidenceeνeν ppp

nnn CdCdCd

e+ee++ e-ee-- γγγ

γγγ

γγγ


Inverse beta decayInverse beta decayof chlorineof chlorine

600 tons of600 tons ofPerchloroethylenePerchloroethylene

Homestake solar neutrinoHomestake solar neutrinoobservatory (1967observatory (1967−−2002)2002)

First Measurement of Solar NeutrinosFirst Measurement of Solar Neutrinos


Cherenkov EffectCherenkov EffectCherenkov Effect

WaterWater

Elastic scattering or Elastic scattering or CC reactionCC reaction

Neutrino

NeutrinoLightLight

LightLight

Cherenkov Cherenkov RingRing

Electron or MuonElectron or Muon(Charged Particle)(Charged Particle)


SuperSuper--Kamiokande: Sun in the Light of NeutrinosKamiokande: Sun in the Light of Neutrinos


John BahcallJohn Bahcall1934 1934 −− 20052005

Raymond Davis Jr.Raymond Davis Jr.1914 1914 −− 20062006

Missing Neutrinos from the SunMissing Neutrinos from the Sun

HomestakeHomestake

ChlorineChlorine

77BeBe

88BB

CNOCNO

Measurement (1970Measurement (1970 –– 1995)1995)

Calculation of expectedCalculation of expectedexperimental countingexperimental countingrate from variousrate from varioussource reactionssource reactions


Neutrino Flavor OscillationsNeutrino Flavor Oscillations

TwoTwo--flavor mixingflavor mixing ⎟⎠

⎞⎜⎝

⎛νν

⎟⎠

⎞⎜⎝

⎛θθ−θθ

=⎟⎟⎠

⎞⎜⎜⎝

⎛νν

μ 2

1ecossinsincos

⎟⎠

⎞⎜⎝

⎛νν

⎟⎠

⎞⎜⎝

⎛θθ−θθ

=⎟⎟⎠

⎞⎜⎜⎝

⎛νν

μ 2

1ecossinsincos

Bruno PontecorvoBruno Pontecorvo(1913 (1913 –– 1993)1993)

Invented nu oscillationsInvented nu oscillations

Each mass eigenstate propagates asEach mass eigenstate propagates as

with with

ipzeipze

E2m

EmEp2

22 −≈−=E2

mEmEp

222 −≈−=

zE2

m2δ zE2

m2δPhase difference implies flavor oscillationsPhase difference implies flavor oscillations

Oscillation Oscillation LengthLength ⎟

⎟⎠

⎞⎜⎜⎝

⎛

δ⎟⎠⎞

⎜⎝⎛=

δ

π2

2

2 m

eVMeV

Em5.2

m

E4⎟⎟⎠

⎞⎜⎜⎝

⎛

δ⎟⎠⎞

⎜⎝⎛=

δ

π2

2

2 m

eVMeV

Em5.2

m

E4

sinsin22(2(2θθ))

ProbabilityProbability ννee →→ ννμμ

zz


ThreeThree--Flavor Neutrino ParametersFlavor Neutrino Parameters

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

ννν

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛−

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

−=

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

ννν

τ

μ

3

2

1

1212

1212

1313

1313

2323

2323

e

1CSSC

CS1

SC

CSSC

1

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

ννν

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛−

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

−=

⎟⎟⎟

⎠

⎞

⎜⎜⎜

⎝

⎛

ννν

τ

μ

3

2

1

1212

1212

1313

1313

2323

2323

e

1CSSC

CS1

SC

CSSC

1 δ−ie δ−ie

δ− ie δ− ie

.,etccosC 1212 θ= .,etccosC 1212 θ= δ δ CPCP--violating phaseviolating phase

SolarSolar7575−−9292

AtmosphericAtmospheric14001400−−30003000

22 meVmΔ 22 meVmΔ

CHOOZCHOOZ Solar/KamLANDSolar/KamLAND 22σσ rangesrangeshephep--ph/0405172ph/0405172

Atmospheric/K2KAtmospheric/K2Koo 5437 23 <θ< oo 5437 23 <θ< o1113 <θ o1113 <θ oo 3630 12 <θ< oo 3630 12 <θ<

μμee ττ

μμee ττ

μμ ττ

11SunSun

NormalNormal

22

33

AtmosphereAtmosphere

μμee ττ

μμee ττ

μμ ττ

11SunSun

InvertedInverted22

33

AtmosphereAtmosphere

Tasks and Open QuestionsTasks and Open Questions

•• Precision for Precision for θθ12 12 andand θθ2323•• How large is How large is θθ1313??•• CPCP--violating phase violating phase δδ??•• Mass orderingMass ordering? ?

(normal vs inverted)(normal vs inverted)•• Absolute massesAbsolute masses ??

(hierarchical vs degenerate)(hierarchical vs degenerate)•• Dirac or MajoranaDirac or Majorana??


“Weighing” Neutrinos with KATRIN“Weighing” Neutrinos with KATRIN

•• Sensitive to Sensitive to common mass scale mcommon mass scale mfor all flavors because of small massfor all flavors because of small massdifferences from oscillationsdifferences from oscillations

•• Best limit from Mainz und TroitskBest limit from Mainz und Troitskm 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://wwwhttp://www--ik.fzk.de/katrin/ik.fzk.de/katrin/


“KATRIN Approaching” (25 Nov 2006)“KATRIN Approaching” (25 Nov 2006)


Neutrino Thermal EquilibriumNeutrino Thermal Equilibrium

Cosmic expansion rateCosmic expansion rate

Friedmann equationFriedmann equation

2Plm

23

8H ρπ

= 2Plm

23

8H ρπ

=

4T~ρ 4T~ρ

Pl

2

mT~HPl

2

mT~H

Radiation dominatesRadiation dominates

Expansion rateExpansion rate

Condition for thermal equilibrium: Condition for thermal equilibrium: ΓΓ > 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 MeV1 MeVcorresponding to t corresponding to t ≲≲ 1 sec1 sec

ν+ν↔+ −+ ee ν+ν↔+ −+ ee

Neutrino reactionsNeutrino reactions

Dimensional analysis of reaction rateDimensional analysis of reaction rateif T if T ≪≪ mmW,ZW,Z

52FTG~Γ 52FTG~Γ

Examples for neutrino processesExamples for neutrino processes

ν+ν↔ν+ν ν+ν↔ν+ν±± +ν↔+ν ee ±± +ν↔+ν ee

GGFF


Thermal RadiationsThermal Radiations

General General Bosons Bosons Fermions Fermions

Energy density Energy density ρρ1e

E

)2(

pdg TE

p3

3

p ±⎮⌡

⌠

π

r

1e

E

)2(

pdg TE

p3

3

p ±⎮⌡

⌠

π

r4

2B T

30g

π 42

B T30

gπ 4

2F T

30g

87 π 4

2F T

30g

87 π

Pressure P Pressure P 3ρ3ρ

Number density n Number density n 1e

1

)2(

pdg TE3

3

p ±⎮⌡

⌠

π

r

1e

1

)2(

pdg TE3

3

p ±⎮⌡

⌠

π

r3

23

B Tgπ

ζ 323

B Tgπ

ζ 323

F Tg43

π

ζ 323

F Tg43

π

ζ

Entropy density s Entropy density s T3

4T

P ρ=

+ρT3

4T

P ρ=

+ρ 32

B T45

2g

π 32

B T45

2g

π 32

F T45

2g

87 π 3

2F T

452

g87 π


PresentPresent--Day Neutrino DensityDay Neutrino Density

Neutrino decouplingNeutrino decoupling(freeze out)(freeze out)

H = H = ΓΓT T ≈≈ 2.4 MeV2.4 MeV (electron flavor)(electron flavor)T T ≈≈ 3.7 MeV3.7 MeV (other flavors)(other flavors)

Redshift of FermiRedshift of Fermi--DiracDiracdistribution (“nothingdistribution (“nothingchanges at freezechanges at freeze--out”)out”) 1e

E1dE

dNT/E

2

2 +π=νν

1e

E1dE

dNT/E

2

2 +π=νν

TemperatureTemperaturescales with redshiftscales with redshiftTTνν = T= Tγγ ∝∝ (z+1)(z+1)

ElectronElectron--positronpositronannihilation beginning annihilation beginning at T at T ≈≈ mmee = 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 photonstransfered to photons

after3

before3 TgTg γ∗γ∗ =

after3

before3 TgTg γ∗γ∗ =

876

42 87+876

42 87+

}2}2 before

3114

after3 TT γγ =

before3

114

after3 TT γγ =

⎪⎭

⎪⎬

⎫

⎪⎭

⎪⎬

⎫

Redshift ofRedshift ofneutrino and photonneutrino and photonthermal distributionsthermal distributionsso that today we haveso that today we have

3113

43

114 cm112nn)flavor1(n −≈=××= γγνν

3113

43

114 cm112nn)flavor1(n −≈=××= γγνν

K95.1T114

T31

≈⎟⎠⎞

⎜⎝⎛= γν K95.1T114

T31

≈⎟⎠⎞

⎜⎝⎛= γν for massless neutrinosfor massless neutrinos


Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses

A classic paper:A classic paper:GershteinGershtein & & ZeldovichZeldovichJETP JETP LettLett. 4 (1966) 120. 4 (1966) 120

4.0eV5.92

mh2 <= ∑ ν

νΩ 4.0eV5.92

mh2 <= ∑ ν

νΩ

Cosmic neutrino “sea”Cosmic neutrino “sea” ~ 112 cm~ 112 cm--33 neutrinos + antineutrinos + anti--neutrinos per flavorneutrinos per flavor

mmνν ≲≲ 40 40 eVeV For allFor allstable flavorsstable flavors


Weakly Interacting Particles as Dark MatterWeakly Interacting Particles as Dark Matter

However, the idea ofHowever, the idea ofweakly interacting massiveweakly interacting massiveparticles as dark matterparticles as dark matteris now standardis now standard

•• More than 30 years ago,More than 30 years ago,beginnings of the idea ofbeginnings of the idea ofweakly interacting particlesweakly interacting particles(neutrinos) as dark matter(neutrinos) as dark matter

•• Massive neutrinos are noMassive neutrinos are nolonger a good candidatelonger a good candidate(hot dark matter)(hot dark matter)


What is wrong with neutrino dark matter?What is wrong with neutrino dark matter?

Galactic Phase Space (“Galactic Phase Space (“TremaineTremaine--GunnGunn--Limit”)Limit”)

mmνν >> 20 20 −− 40 40 eVeV

2

3escape

n

2

3max

max3

)vm(m

3

pm

max

π=

π=ρ νν

ν321

2

3escape

n

2

3max

max3

)vm(m

3

pm

max

π=

π=ρ νν

ν321

Maximum mass density of a degenerateMaximum mass density of a degenerateFermi gasFermi gas

mmνν >> 100 100 −− 200 200 eVeV

SpiralSpiralgalaxiesgalaxies

DwarfDwarfgalaxiesgalaxies

•• NusNus are “Hot Dark Matter”are “Hot Dark Matter”•• Ruled out Ruled out

by structure formationby structure formation

Neutrino Free Streaming (Neutrino Free Streaming (CollisionlessCollisionless Phase Mixing)Phase Mixing)

•• AtAt TT << 11 MeVMeV neutrinoneutrino scatteringscattering inin earlyearly universeuniverse ineffectiveineffective•• Stream freely untilStream freely until nonnon--relativisticrelativistic•• Wash out density contrasts on small scales Wash out density contrasts on small scales

NeutrinosNeutrinosNeutrinosNeutrinos

OverOver--densitydensity


Structure Formation in the UniverseStructure Formation in the Universe

SmoothSmooth StructuredStructured

Structure forms byStructure forms bygravitational instabilitygravitational instabilityof primordialof primordialdensity fluctuationsdensity fluctuations


Structure Formation in the UniverseStructure Formation in the Universe

SmoothSmooth StructuredStructured

Structure forms byStructure forms bygravitational instabilitygravitational instabilityof primordialof primordialdensity fluctuationsdensity fluctuations

A fraction of hot dark matter A fraction of hot dark matter suppresses smallsuppresses small--scale structurescale structure


Neutrino Free Streaming Neutrino Free Streaming −− Transfer FunctionTransfer Function

Hannestad, Neutrinos in Cosmology, hepHannestad, Neutrinos in Cosmology, hep--ph/0404239ph/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 −− 88ΩΩνν//ΩΩM M

valid forvalid for

88ΩΩνν//ΩΩM M ≪≪ 11

Power suppression for Power suppression for λλFSFS ≳≳ 100 Mpc/h100 Mpc/h

mmνν = 0= 0

mmνν = 0.3 eV= 0.3 eV

mmνν = 1 eV= 1 eV


Power Spectrum of Cosmic Density FluctuationsPower Spectrum of Cosmic Density Fluctuations


Some Recent Cosmological Limits on Neutrino MassesSome Recent Cosmological Limits on Neutrino Masses

ΣΣmmνν/eV/eV(limit 95%CL)(limit 95%CL) Data / PriorsData / Priors

Spergel et al. (WMAP) 2003Spergel et al. (WMAP) 2003[astro[astro--ph/0302209] ph/0302209] 0.690.69 WMAPWMAP--1, 2dF, HST, 1, 2dF, HST, σσ88

Hannestad 2003Hannestad 2003[astro[astro--ph/0303076]ph/0303076] 1.011.01 WMAPWMAP--1, CMB, 2dF, HST1, CMB, 2dF, HST

Crotty et al. 2004Crotty et al. 2004[hep[hep--ph/0402049]ph/0402049]

1.01.00.60.6

WMAPWMAP--1, CMB, 2dF, SDSS1, CMB, 2dF, SDSS& HST, SN& HST, SN

Hannestad 2004Hannestad 2004[hep[hep--ph/0409108]ph/0409108] 0.650.65 WMAPWMAP--1, SDSS, SN Ia gold sample,1, SDSS, SN Ia gold sample,

LyLy--αα data from Keck sample data from Keck sample

Seljak et al. 2004Seljak et al. 2004[[astroastro--ph/0407372]ph/0407372] 0.420.42 WMAPWMAP--1, SDSS, Bias,1, SDSS, Bias,

LyLy--αα data from SDSS sample data from SDSS sample

Spergel et al. 2006Spergel et al. 2006[hep[hep--ph/0409108]ph/0409108] 0.680.68 WMAPWMAP--3, SDSS, 2dF, SN Ia, 3, SDSS, 2dF, SN Ia, σσ88

Seljak et al. 2006Seljak et al. 2006[astro[astro--ph/0604335]ph/0604335] 0.140.14 WMAPWMAP--3, CMB3, CMB--small, SDSS, 2dF,small, SDSS, 2dF,

SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), LyLy--αα (SDSS)(SDSS)

Hannestad et al. 2006Hannestad et al. 2006[hep[hep--ph/0409108]ph/0409108] 0.300.30 WMAPWMAP--1, CMB1, CMB--small, SDSS, 2dF,small, SDSS, 2dF,

SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), LyLy--αα (SDSS)(SDSS)


Weak Lensing Weak Lensing −− A Powerful Probe for the FutureA Powerful Probe for the Future

UnlensedUnlensed LensedLensed

Distortion of background images by foreground matterDistortion of background images by foreground matter


Sensitivity Forecasts for Future LSS ObservationsSensitivity Forecasts for Future LSS Observations

Kaplinghat, Knox & Song,Kaplinghat, Knox & Song,astroastro--ph/0303344ph/0303344

σσ(m(mνν) ~ 0.15 eV ) ~ 0.15 eV (Planck)(Planck)

σσ(m(mνν) ~ 0.044 eV (CMBpol)) ~ 0.044 eV (CMBpol)CMB lensingCMB lensing

LesgourguesLesgourgues, , PastorPastor& & PerottoPerotto,,hephep--ph/0403296 ph/0403296

Planck & SDSSPlanck & SDSS ΣΣmmνν > 0.21 eV detectable> 0.21 eV detectableat 2at 2σσ

ΣΣmmνν > 0.13 eV detectable> 0.13 eV detectableat 2at 2σσ

Ideal CMB & 40 x SDSSIdeal CMB & 40 x SDSS

Abazajian & DodelsonAbazajian & Dodelsonastroastro--ph/0212216ph/0212216

Future weak lensingFuture weak lensingsurvey 4000 degsurvey 4000 deg22 σσ(m(mνν) ~ 0.1 eV) ~ 0.1 eV

WangWang, , HaimanHaiman, , HuHu, , KhouryKhoury & & MayMay,,astroastro--ph/0505390ph/0505390

WeakWeak--lensing selectedlensing selectedsample of > 10sample of > 105 5 clustersclusters σσ(m(mνν) ~ 0.03 eV) ~ 0.03 eV

Hannestad, Tu & WongHannestad, Tu & Wongastroastro--ph/0603019ph/0603019

WeakWeak--lensing tomographylensing tomography(LSST plus Planck)(LSST plus Planck) σσ(m(mνν) ~ 0.05 eV) ~ 0.05 eV


FermionFermion Mass SpectrumMass 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 μμ ττ

All flavorsAll flavors

νν33NeutrinosNeutrinos


TitleTitle


NeutrinosNeutrinos0.10.1−−2%2%Dark MatterDark Matter

23%23%

Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about10% luminous) 10% luminous)




++2/32/3

cc

tt



Strong Int’n Strong Int’n

Electromagnetic Int’nElectromagnetic Int’n

−−1/3 1/3

ss

bb

−−1 1

μμ

0 0

11stst FamilyFamily

22ndnd Family Family

33rdrd FamilyFamily

uu dd ee eνeν

μνμν

ττ τντν

ChargeCharge 0 0

MatterMatter

AntiAnti--QuarksQuarksAntiAnti--LeptonsLeptons

−−2/32/3++1/3 1/3 0 0 ++1 1

eνeν +e+e dd uu

μνμν

τντν

+μ+μ+τ+τ

ss

bb

cc

tt

Strong Int’nStrong Int’n


AntimatterAntimatter

Why is there no antimatterWhy is there no antimatterin the Universe?in the Universe?

(Problem of „Baryogenesis”)(Problem of „Baryogenesis”)




++2/32/3

cc

tt



Strong Int’n Strong Int’n


−−1/3 1/3

ss

bb

−−1 1

μμ

0 0

11stst FamilyFamily

22ndnd Family Family

33rdrd FamilyFamily

uu dd ee eνeν

μνμν

ττ τντν

ChargeCharge 0 0

MatterMatter

AntiAnti--QuarksQuarksAntiAnti--LeptonsLeptons

−−2/32/3++1/3 1/3 0 0 ++1 1

eνeν +e+e dd uu

μνμν

τντν

+μ+μ+τ+τ

ss

bb

cc

tt

Strong Int’nStrong Int’n


AntimatterAntimatter

Why is there no antimatterWhy is there no antimatterin the Universe?in the Universe?

(Problem of „Baryogenesis”)(Problem of „Baryogenesis”)

0 0

eνeν

μνμν

τντν

00

LeptonsLeptons AntiAnti--LeptonsLeptons

„Majorana Neutrinos”„Majorana Neutrinos”are their ownare their ownantiparticlesantiparticles

Can explain baryogenesisCan explain baryogenesisby leptogenesisby leptogenesis


BaryogenesisBaryogenesis in the Early Universein the Early Universe

SakharovSakharov conditions for creating the conditions for creating the BBaryon aryon AAsymmetry of the symmetry of the UUniverse (niverse (BAUBAU))•• C and CP violationC and CP violation•• Baryon number violationBaryon number violation•• Deviation from thermal equilibriumDeviation from thermal equilibrium

ParticleParticle--physics standard modelphysics standard model•• Violates C and CPViolates C and CP•• Violates B and L by EWViolates B and L by EW instantoninstanton effectseffects

(B (B −− L conserved)L conserved)

•• However, electroweak baryogenesis not quantitativelyHowever, electroweak baryogenesis not quantitativelypossible within particlepossible within particle--physics standard modelphysics standard model

•• Works in SUSY models for small range of parametersWorks in SUSY models for small range of parameters

Andrei SakharovAndrei Sakharov19211921−−19891989

A.Riotto & M.Trodden: A.Riotto & M.Trodden: Recent progress in baryogenesis Recent progress in baryogenesis Ann. Rev. Nucl. Part. Sci. 49 (1999) 35Ann. Rev. Nucl. Part. Sci. 49 (1999) 35


NeutrinosNeutrinosCharged LeptonsCharged Leptons

SeeSee--Saw Model for Neutrino MassesSaw Model for Neutrino Masses

DiagonalizeDiagonalize

Lagrangian for Lagrangian for particle massesparticle masses =massL =massL .c.h+ .c.h+

DiracDirac massesmassesfrom couplingfrom couplingto standardto standardHiggs field Higgs field φφ

RLRL Ngeg νφ−φ− ll l RLRL Ngeg νφ−φ− ll l

HeavyHeavyMajoranaMajoranamassesmassesMMjj > 10> 101010 GeVGeV

RcR2

1 MNN− RcR2

1 MNN−

( ) ⎟⎠

⎞⎜⎝

⎛ ν⎟⎟⎠

⎞⎜⎜⎝

⎛φ

φν

ν

ν

R

LRL NMg

g0N( ) ⎟

⎠

⎞⎜⎝

⎛ ν⎟⎟⎠

⎞⎜⎜⎝

⎛φ

φν

ν

ν

R

LRL NMg

g0N ( ) ⎟

⎠

⎞⎜⎝

⎛ ν

⎟⎟⎟⎟

⎠

⎞

⎜⎜⎜⎜

⎝

⎛ φ

νν

R

L

22

RL NM0

0M

g

N( ) ⎟⎠

⎞⎜⎝

⎛ ν

⎟⎟⎟⎟

⎠

⎞

⎜⎜⎜⎜

⎝

⎛ φ

νν

R

L

22

RL NM0

0M

g

N

Light Majorana massLight Majorana mass

Mg 22 φν

Mg 22 φν


SeeSee--Saw Model for Neutrino MassesSaw Model for Neutrino Masses

( ) ⎟⎠

⎞⎜⎝

⎛ ν

⎟⎟⎟⎟

⎠

⎞

⎜⎜⎜⎜

⎝

⎛ φ

νν

R

L

22

RL NM0

0M

g

N( ) ⎟⎠

⎞⎜⎝

⎛ ν

⎟⎟⎟⎟

⎠

⎞

⎜⎜⎜⎜

⎝

⎛ φ

νν

R

L

22

RL NM0

0M

g

N

Light Majorana massLight Majorana mass

Mg 22 φν

Mg 22 φν

N

νℓ±

10101010 GeVGeV 11 GeVGeV 1010−−1010 GeVGeV

ChargedChargedleptonsleptons

OrdinaryOrdinaryneutrinosneutrinos

HeavyHeavy“right“right--handed”handed”neutrinosneutrinos(no gauge(no gaugeinteractions)interactions)


EquilibriumEquilibriumabundance ofabundance ofheavy Majoranaheavy Majorananeutrinosneutrinos

W. Buchmüller & M. Plümacher: Neutrino masses and the baryon asyW. Buchmüller & M. Plümacher: Neutrino masses and the baryon asymmetrymmetryInt. J. Mod. Phys. A15 (2000) 5047Int. J. Mod. Phys. A15 (2000) 5047--50865086

M. Fukugita & T. Yanagida:M. Fukugita & T. Yanagida:Baryogenesis without GrandBaryogenesis without GrandUnificationUnificationPhys. Lett. B 174 (1986) 45 Phys. Lett. B 174 (1986) 45

Leptogenesis by OutLeptogenesis by Out--ofof--Equilibrium DecayEquilibrium Decay


Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate

CreatedCreatedleptonlepton--numbernumberabundanceabundance


Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate

CPCP--violating decays byviolating decays byinterference of treeinterference of tree--levellevelwith onewith one--loop diagramloop diagram

πν=Γ 8M2

Decay g πν=Γ 8M2

Decay g


LeptogenesisLeptogenesis by by MajoranaMajorana Neutrino DecaysNeutrino Decays

In seeIn see--saw models for neutrino masses, outsaw models for neutrino masses, out--ofof--equilibriumequilibriumdecays of rightdecays of right--handed heavy handed heavy MajoranaMajorana neutrinos provideneutrinos providesource for CPsource for CP-- and Land L--violationviolation

Cosmological evolutionCosmological evolution•• B = L = 0 early onB = L = 0 early on•• Thermal freezeThermal freeze--out of heavy out of heavy MajoranaMajorana neutrinosneutrinos•• OutOut--ofof--equilibrium CPequilibrium CP--violating decay creates net Lviolating decay creates net L•• Shift L excess into B byShift L excess into B by sphaleronsphaleron effectseffects

Sufficient deviation from Sufficient deviation from equilibrium distribution of equilibrium distribution of heavy heavy MajoranaMajorana neutrinos neutrinos at freezeat freeze--outout

Limits onLimits onYukawaYukawacouplingscouplings

Limits onLimits onmasses ofmasses ofordinaryordinaryneutrinosneutrinos

Requires Majorana neutrino masses below 0.1 Requires Majorana neutrino masses below 0.1 eVeVBuchmüller, Di Bari & Plümacher, hepBuchmüller, Di Bari & Plümacher, hep--ph/0209301 & hepph/0209301 & hep--ph/0302092ph/0302092


TitleTitle


NeutrinosNeutrinos0.10.1−−2%2%Dark MatterDark Matter

23%23%

Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about10% luminous) 10% luminous)



4. Candidates and Searchesfor Particle Dark Matter

4. Candidates and Searchesfor Particle Dark Matter




LeeLee--WeinbergWeinberg--CurveCurve

Weakly interacting Weakly interacting massive particlesmassive particles(WIMPs) possible as (WIMPs) possible as cold dark mattercold dark matter

•• For mFor mνν ≳≳ 1 MeV1 MeVneutrinos freeze outneutrinos freeze outnonrelativisticallynonrelativistically

•• Density suppressedDensity suppressedby annihilationby annihilationbefore freezebefore freeze--outout


Survival of the WeakestSurvival of the Weakest

Boltzmann suppressionBoltzmann suppressionof equilibrium densityof equilibrium densityn n ∝∝ exp(exp(−−m/T)m/T)

Number density freezesNumber density freezesout when annihilationout when annihilationrate is slower thanrate is slower thancosmic expansion ratecosmic expansion rate

GondoloGondoloastroastro--ph/0403064ph/0403064


Electroweak Scale FavoredElectroweak Scale Favored ??

)nn(vHn3dtdn 2

eq2

A −σ−=+ )nn(vHn3dtdn 2

eq2

A −σ−=+

vtermsarithmiclog

factorshA

2σ

×=Ωv

termsarithmiclogfactorsh

A

2σ

×=Ω

22

mGeV01

11.0h ⎟⎠⎞

⎜⎝⎛≈Ω

22

mGeV01

11.0h ⎟⎠⎞

⎜⎝⎛≈Ω

Boltzmann collision equation forBoltzmann collision equation fornumber density n of particlesnumber density n of particleswith annihilation cross section with annihilation cross section σσAA

Resulting cosmic mass densityResulting cosmic mass density

Concordance dark matter densityConcordance dark matter density 006.0110.0h2 ±=Ω 006.0110.0h2 ±=Ω

Mass for Mass for WWeakly eakly IInteracting nteracting MMassiveassivePParticle (WIMP) as dark matter article (WIMP) as dark matter

GeV10m ≈ GeV10m ≈

With electroweak cross sectionWith electroweak cross section(Majorana neutrino)(Majorana neutrino)

Cosmic dark matter density of thermal relicsCosmic dark matter density of thermal relicsand approximate electroweak gauge coupling and approximate electroweak gauge coupling strengthstrengthfavor electroweak scale for scale of new phyfavor electroweak scale for scale of new physicssics


Supersymmetric Extension of Particle PhysicsSupersymmetric Extension of Particle Physics

In supersymmetric extensions of the particleIn supersymmetric extensions of the particle--physics standard model,physics standard model,every boson has a fermionic partner and vice versaevery boson has a fermionic partner and vice versa

SleptonsSleptons (e,(e, ννee, …), …)SquarksSquarks (u, d, …)(u, d, …)

SpinSpinSuperpartnerSuperpartner

00

1/21/2GluinosGluinosWinoWinoZinoZinoPhotinoPhotino ((γγ))

1/21/2

3/23/2

HiggsinoHiggsino

GravitinoGravitino

~~

~~ ~~~~~~

•• If RIf R--Parity is conserved, the lightestParity is conserved, the lightest SUSYSUSY--particle (LSP) isparticle (LSP) is stablestable•• Most plausible candidateMost plausible candidate forfor dark matter is the neutralino,dark matter is the neutralino,

similar to a massive Majoranasimilar to a massive Majorana neutrinoneutrino

NeutralinoNeutralino = C= C11 PhotinoPhotino + C+ C22 ZinoZino + C+ C33 HiggsinoHiggsino

1/21/2 Leptons (e,Leptons (e, ννee, …), …)Quarks (u, d, …)Quarks (u, d, …)

11 GluonsGluonsWW±±

ZZ00

Photon (Photon (γγ))

00

22

HiggsHiggs

GravitonGraviton

SpinSpin Standard particleStandard particle


“Inventors”“Inventors” of Superof Super--SymmetrySymmetry

Julius Wess (1934Julius Wess (1934−−2007)2007)Director emeritus MPI PhysicsDirector emeritus MPI Physics

Bruno ZuminoBruno Zumino(born 1923)(born 1923)


SUSY Particles Natural as Dark MatterSUSY Particles Natural as Dark Matter ??

Gondolo, astroGondolo, astro--ph/0403064ph/0403064


Dark SUSYDark SUSY


Killing Two Birds with One StoneKilling Two Birds with One Stone

A “good” particleA “good” particledark matter candidate isdark matter candidate ismotivated by solving anmotivated by solving anissue in particle physicsissue in particle physics

SupersymmetrySupersymmetry•• Solves hierarchy problemSolves hierarchy problem•• Can provide dark matterCan provide dark matter


The Search for Dark Matter in our GalaxyThe Search for Dark Matter in our Galaxy

(With permission of David Simmonds ©)


Search for Neutralino Dark MatterSearch for Neutralino Dark Matter

Direct Method (Laboratory Experiments)

CrystalCrystalEnergyEnergydepositiondeposition

Recoil energyRecoil energy(few keV) is(few keV) ismeasured bymeasured by•• IonisationIonisation•• ScintillationScintillation•• CryogenicCryogenic

GalacticGalacticdark matterdark matterparticleparticle(e.g.neutralino)(e.g.neutralino)


WIMP SearchesWIMP Searches

COUPPCOUPPPICASSOPICASSO

XENONXENONLUX, ZEPLINLUX, ZEPLINWARP, ArDMWARP, ArDM

DEAP/CLEANDEAP/CLEANDAMA/LIBRADAMA/LIBRAKIMS, XMASSKIMS, XMASS

DRIFTDRIFTGERDAGERDA

CDMSCDMSEDELWEISSEDELWEISS

CRESSTCRESSTROSEBUDROSEBUD

HeatHeatPhononsPhonons

ChargeCharge LightLight


Underground PhysicsUnderground Physics

Gran Sasso Laboratory (Italy)Gran Sasso Laboratory (Italy)

Background suppression most crucialBackground suppression most crucialrequirement for WIMP searches.requirement for WIMP searches.Underground Labs: Shield cosmic raysUnderground Labs: Shield cosmic rays


CRESST Experiment to Search for Dark MatterCRESST Experiment to Search for Dark Matter


The DAMA/LIBRA Experiment in the Gran SassoThe DAMA/LIBRA Experiment in the Gran Sasso

5 x 5 crystals à 9.7 kg10.2 × 10.2 × 25.4 cm3

PMT+ HV divider

~ 1 event/keV/kg/d~ 1 event/keV/kg/d

WIMP contribution at low energies?WIMP contribution at low energies?

Data since Sep 2003Data since Sep 20030.53 0.53 ton x yearston x years


DAMA/LIBRA Evidence for WIMP DetectionDAMA/LIBRA Evidence for WIMP Detection

DAMA/LIBRA experiment in Gran Sasso (NaI scintillationDAMA/LIBRA experiment in Gran Sasso (NaI scintillationdetector) observes an annual modulation at adetector) observes an annual modulation at a8.28.2σσ statistical CL, based on statistical CL, based on 0.82 ton0.82 ton--years of data years of data [[Riv. N. Cim. 26 (2003) 1Riv. N. Cim. 26 (2003) 1−−7373, , arXiv:0804.2741 (2008)]arXiv:0804.2741 (2008)]

• Detector stability ?• „Background stability“ ?


Limits and Forecasts for Direct WIMP SearchesLimits and Forecasts for Direct WIMP Searches


Search for Neutralino Dark MatterSearch for Neutralino Dark Matter

Direct Method (Laboratory Experiments)

CrystalCrystalEnergyEnergydepositiondeposition

Recoil energyRecoil energy(few keV) is(few keV) ismeasured bymeasured by•• IonisationIonisation•• ScintillationScintillation•• CryogenicCryogenic

GalacticGalacticdark matterdark matterparticleparticle(e.g.neutralino)(e.g.neutralino)

Indirect Method (Neutrino Telescopes)

SunSun

Galactic darkGalactic darkmattermatterparticlesparticlesare accretedare accreted

AnnihilationAnnihilationHighHigh--energy energy neutrinosneutrinos((GeVGeV--TeVTeV))can be measuredcan be measured


IceCube Neutrino Telescope at the South PoleIceCube Neutrino Telescope at the South Pole

•• 1 km1 km33 antarctic ice, instrumentedantarctic ice, instrumentedwith 4800 photomultiplierswith 4800 photomultipliers

•• 40 of 80 strings installed (2008)40 of 80 strings installed (2008)•• Completion until 2011 foreseenCompletion until 2011 foreseen


ANTARES ANTARES −− Neutrino Telescope in the MediterraneanNeutrino Telescope in the Mediterranean


Luminous Creatures of the Deep OceanLuminous Creatures of the Deep Ocean


Sensitivity of IceCube to SUSY Dark MatterSensitivity of IceCube to SUSY Dark Matter

With Deep Core addition

J. Edsjö, 2007

Rates Rates computedcomputedwithwith


Can We See the Dark Matter?Can We See the Dark Matter?

HESS airshowerHESS airshowertelescope, Namibiatelescope, Namibia

MAGIC, La PalmaMAGIC, La Palma

GLAST SatelliteGLAST SatelliteLaunch 11 June 08Launch 11 June 08

Dark matter particles canDark matter particles candirectly annihilatedirectly annihilate

The dark halo of our galaxyThe dark halo of our galaxycan slightly glow incan slightly glow inhighhigh--energy gamma raysenergy gamma rays

γγ→χχ γγ→χχ


Substructure in Dark Matter HalosSubstructure in Dark Matter Halos

Millenium SimulationMillenium Simulation

On small scales, dark matterOn small scales, dark matterin numerical simulations isin numerical simulations isfound to be very “clumpy”found to be very “clumpy”

•• Facilitates dark matterFacilitates dark matterannihilationannihilation(boost factor for (boost factor for γγ raysrays22−−15 from subhalos)15 from subhalos)

•• Where are the dwarf galaxiesWhere are the dwarf galaxiesin our Milky Way?in our Milky Way?

•• Problem for standardProblem for standardcold dark matter scenario?cold dark matter scenario?


HighHigh--Energy Gamma Rays from Neutralino AnnihilationEnergy Gamma Rays from Neutralino Annihilation

Stoehr et al.,astro-ph/0307026

Bergstöm, Ullio & Buckley,astro-ph/9712318

γγγ→χχ Zor γγγ→χχ Zor


GLAST Sensitivity after 1 YearGLAST Sensitivity after 1 Year

GLAST working group on Dark Matter andGLAST working group on Dark Matter andNew Physics, E. Baltz & al., JCAP, 2008New Physics, E. Baltz & al., JCAP, 2008

Conservative approach:Conservative approach:•• Galactic centerGalactic center•• NFW halo profile assumedNFW halo profile assumed•• No substructureNo substructure

Vast region of opportunityVast region of opportunityfor next generation offor next generation ofgammagamma--ray instrumentsray instruments

Estimate including all haloEstimate including all halowith substructurewith substructure(L. Bergstr(L. Bergströömm))


Search for SUSY with the Large Hadron Collider (LHC)Search for SUSY with the Large Hadron Collider (LHC)

LHC at CERN (Geneva)LHC at CERN (Geneva)Operation beginning 2008Operation beginning 2008

•• Protons will collide with theProtons will collide with thelargest energies ever in the lablargest energies ever in the lab(but larger ones in cosmic rays) (but larger ones in cosmic rays)

•• Discovery of new particlesDiscovery of new particlesexpected, such as Higgs particlesexpected, such as Higgs particlesor supersymmetric partners toor supersymmetric partners toordinary matterordinary matter


Simulation or a ProtonSimulation or a Proton--Proton Collision at the LHC Proton Collision at the LHC

LHC at CERN (Geneva)LHC at CERN (Geneva)Operation beginning 2008Operation beginning 2008


Hunting WIMPsHunting WIMPs

Search for new particles at accelerators,Search for new particles at accelerators,notably the Large Hadron Collider (LHC)notably the Large Hadron Collider (LHC)at CERN (> 2008)at CERN (> 2008)

Search for WIMP annihilation products in the form ofSearch for WIMP annihilation products in the form of•• Gamma rays (e.g. EGRET, HESS, MAGIC, GLAST)Gamma rays (e.g. EGRET, HESS, MAGIC, GLAST)•• AntiAnti--protons (AMS, Pamela)protons (AMS, Pamela)•• Positrons (AMS, Pamela)Positrons (AMS, Pamela)•• HighHigh--energy neutrinos from the Sun or Earthenergy neutrinos from the Sun or Earth

(e.g. Super(e.g. Super--K, Amanda/IceCube, Antares, …)K, Amanda/IceCube, Antares, …)

Recoil energyRecoil energy(few keV) is(few keV) ismeasured bymeasured by•• IonisationIonisation•• ScintillationScintillation•• CryogenicallyCryogenically


Axion Physics in a Nut ShellAxion Physics in a Nut Shell

CosmologyCosmology

CosmicCosmicStringString

In spite of small mass, axionsIn spite of small mass, axionsare born are born nonnon--relativisticallyrelativistically(“non(“non--thermal relics”)thermal relics”)

→→ “Cold dark matter”“Cold dark matter”candidate candidate mmaa ~ 1~ 1--1000 1000 μμeVeV

Search for Axion Dark MatterSearch for Axion Dark Matter

SS

NN

γγaa

BBextext

Microwave resonatorMicrowave resonator(1 GHz (1 GHz == 4 4 μμeV)eV)

PrimakoffPrimakoffconversionconversion

ParticleParticle--Physics MotivationPhysics Motivation

CP conservation in QCD byCP conservation in QCD byPecceiPeccei--Quinn mechanismQuinn mechanism

For fFor faa ≫≫ ffππ axions are “invisible”axions are “invisible”and very lightand very light

→→ AxionsAxions aa ~ ~ ππ00

mmππffππ ≈≈ mmaaffaa

γγ

γγaa

Solar and Stellar AxionsSolar and Stellar Axions

Axions thermally produced in stars,Axions thermally produced in stars,e.g. by Primakoffe.g. by Primakoff productionproduction

•• Limits from avoiding excessiveLimits from avoiding excessiveenergy drainenergy drain

•• SearchSearch forfor solarsolar axionsaxions (CAST, Sumico)(CAST, Sumico)

aaγγ


The Cleansing AxionThe Cleansing Axion

“I named them after a laundry“I named them after a laundrydetergent, since they clean updetergent, since they clean upa problem with an axial current.”a problem with an axial current.”(Nobel lecture 2004, written version)(Nobel lecture 2004, written version)

Frank WilczekFrank Wilczek


Axions as Pseudo NambuAxions as Pseudo Nambu--Goldstone BosonsGoldstone Bosons

•• The realization of the PecceiThe realization of the Peccei--Quinn mechanism involves a new chiral Quinn mechanism involves a new chiral U(1) symmetry, spontaneously broken at a scale fU(1) symmetry, spontaneously broken at a scale faa

•• Axions are the corresponding NambuAxions are the corresponding Nambu--Goldstone modeGoldstone mode

E E ≈≈ ffaa

•• UUPQPQ(1) spontaneously broken (1) spontaneously broken •• Higgs field settles in Higgs field settles in “Mexican hat”“Mexican hat”

aa

V(a)V(a)

E E ≈≈ ΛΛQCD QCD ≪≪ ffaa

•• UUPQPQ(1) explicitly broken (1) explicitly broken byby instantoninstanton effects effects

•• Mexican hat tiltsMexican hat tilts•• AxionsAxions acquire a massacquire a mass

aa

V(a)V(a)

ΘΘ=0=0__


LeeLee--Weinberg Curve for Neutrinos andWeinberg Curve for Neutrinos and AxionsAxions

log(log(ΩΩaa))

log(mlog(maa))

ΩΩMM

1010 eVeV1010 μμeVeV

CDMCDM HDMHDM

AxionsAxions

Thermal RelicsThermal RelicsNonNon--ThermalThermal

RelicsRelics

log(log(ΩΩνν))

log(log(mmνν))

ΩΩMM

1010 eVeV

CDMCDMHDMHDM

1010 GeVGeV

NeutrinosNeutrinos& WIMPs& WIMPs

Thermal RelicsThermal Relics


Search for GalacticSearch for Galactic Axions (Cold Dark Matter)Axions (Cold Dark Matter)

PowerPower

FrequencyFrequency mmaa

AxionAxion SignalSignal

Thermal noise of Thermal noise of cavity & detectorcavity & detector

Power of galacticPower of galactic axionaxion signalsignal

⎟⎟⎠

⎞⎜⎜⎝

⎛

×

ρ⎟⎟⎠

⎞⎜⎜⎝

⎛π

×

⎟⎠⎞

⎜⎝⎛×

−

−

325aa

5

2

321

cm/g105GHz2m

10

QT5.8

B

m22.0

VW104

⎟⎟⎠

⎞⎜⎜⎝

⎛

×

ρ⎟⎟⎠

⎞⎜⎜⎝

⎛π

×

⎟⎠⎞

⎜⎝⎛×

−

−

325aa

5

2

321

cm/g105GHz2m

10

QT5.8

B

m22.0

VW104

Microwave EnergiesMicrowave Energies(1 GHz (1 GHz ≈≈ 44 μμeVeV))

DM axionsDM axionsVelocities in galaxyVelocities in galaxyEnergies thereforeEnergies therefore

mmaa = 1= 1--1000 1000 μμeVeVvvaa ≈≈ 1010−−33 ccEEaa ≈≈ (1(1 ±± 1010−−66) m) maa

Axion HaloscopeAxion Haloscope (Sikivie(Sikivie 1983)1983)

BBextext ≈≈ 8 Tesla8 Tesla

Microwave Microwave ResonatorResonatorQ Q ≈≈ 101055

PrimakoffPrimakoff ConversionConversionγγaa

BBextext

CavityCavityovercomesovercomesmomentummomentummismatchmismatch


ADMX (G.Carosi, Fermilab, May 2007)ADMX (G.Carosi, Fermilab, May 2007)


DirectDirectsearchsearch

Too muchToo muchcold dark mattercold dark matter

TeleTelescopescopeExperimentsExperiments

Globular clustersGlobular clusters(a(a--γγ--coupling)coupling)

Too manyToo manyeventsevents

Too muchToo muchenergy lossenergy loss

SN 1987A (aSN 1987A (a--NN--coupling)coupling)

Axion BoundsAxion Bounds

101033 101066 101099 10101212 [[GeVGeV]] ffaa

eVeVkeVkeV meVmeV μμeVeVmmaa

Too much hot dark matterToo much hot dark matter

CASTCAST ADMXADMX


Some Dark Matter CandidatesSome Dark Matter Candidates

Supersymmetric particlesSupersymmetric particles•• NeutralinosNeutralinos•• AxinosAxinos•• GravitinosGravitinos

Gauge hierarchy problemGauge hierarchy problem

Little Higgs modelsLittle Higgs models

KaluzaKaluza--Klein excitationsKlein excitations Large extra dimensionsLarge extra dimensions

AxionsAxions CP Problem of strong interactionsCP Problem of strong interactions

Sterile neutrinosSterile neutrinos RightRight--handes states should existhandes states should exist

Wimpzillas (superheavy particles)Wimpzillas (superheavy particles) Super GZK cosmic raysSuper GZK cosmic rays

MeVMeV--mass dark mattermass dark matter Explain cosmicExplain cosmic--ray positronsray positrons

Mirror matterMirror matter Exact parity symmetryExact parity symmetry

Primordial black holesPrimordial black holes

QQ--ballsballsWhy notWhy not ??


Hubble Deep FieldHubble Deep Field

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