Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City Geheimnis der dunklen Materie Geheimnis der dunklen Materie Cosmology and the Dark Universe Cosmology and the Dark Universe Georg Raffelt, Max-Planck-Institut für Physik, München Georg Raffelt, Max-Planck-Institut für Physik, München Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico
81
Embed
Cosmology and the Dark Universe · Quarks Leptons Charge +2/3 Up Charge −1/3 Down ... Neutrino Flavor Oscillations Two-flavor mixing ⎟ ... • Massive neutrinos are no longer
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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)?
At Earth 66 billion neutrinos/cmAt Earth 66 billion neutrinos/cm22 secsec
ReactionReaction--chainschains
EnergyEnergy26.7 MeV26.7 MeV
HeliumHelium
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Homestake solar neutrinoHomestake solar neutrinoobservatory (1967observatory (1967−−2002)2002)
First Measurement of Solar NeutrinosFirst Measurement of Solar Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
SuperSuper--Kamiokande: Sun in the Light of NeutrinosKamiokande: Sun in the Light of Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
SuperSuper--Kamiokande: Sun in the Light of NeutrinosKamiokande: Sun in the Light of Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
•• 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??
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
“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
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
•• 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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Structure Formation in the UniverseStructure Formation in the Universe
SmoothSmooth StructuredStructured
Structure forms byStructure forms bygravitational instabilitygravitational instabilityof primordialof primordialdensity fluctuationsdensity fluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Power Spectrum of Cosmic Density FluctuationsPower Spectrum of Cosmic Density Fluctuations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Ordinary Matter 4%Ordinary Matter 4%(of this only about(of this only about10% luminous) 10% luminous)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Periodic System of Elementary ParticlesPeriodic System of Elementary Particles
QuarksQuarks LeptonsLeptons
++2/32/3
cc
tt
Gravitation Gravitation
Weak InteractionWeak Interaction
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
Electromagnetic Int’nElectromagnetic Int’n
AntimatterAntimatter
Why is there no antimatterWhy is there no antimatterin the Universe?in the Universe?
(Problem of „Baryogenesis”)(Problem of „Baryogenesis”)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Periodic System of Elementary ParticlesPeriodic System of Elementary Particles
QuarksQuarks LeptonsLeptons
++2/32/3
cc
tt
Gravitation Gravitation
Weak InteractionWeak Interaction
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
Electromagnetic Int’nElectromagnetic 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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
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
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
•• Density suppressedDensity suppressedby annihilationby annihilationbefore freezebefore freeze--outout
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
•• 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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Dark SUSYDark SUSY
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
The Search for Dark Matter in our GalaxyThe Search for Dark Matter in our Galaxy
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
CRESST Experiment to Search for Dark MatterCRESST Experiment to Search for Dark Matter
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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“ ?
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Limits and Forecasts for Direct WIMP SearchesLimits and Forecasts for Direct WIMP Searches
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
Search for Neutralino Dark MatterSearch for Neutralino Dark Matter
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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?
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
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))
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Escuela Avanzada de Verano, 7-11 July 2008, Cinvestav, Mexico-City
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”