dark matters: wimp and beyond
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Dark Matters: WIMP and Beyond. Shufang Su U. of Arizona SI 2005. Outline. -. Brief introduction of standard cosmology Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM, lightest KK particle in UED - PowerPoint PPT PresentationTRANSCRIPT
Dark Matters:
WIMP and Beyond
Dark Matters:
WIMP and Beyond
Shufang Su Shufang Su
U. of ArizonaU. of Arizona
SI 2005SI 2005
Shufang Su Shufang Su
U. of ArizonaU. of Arizona
SI 2005SI 2005
S. Su Dark Matters 2
Outline Outline
Brief introduction of standard cosmologyBrief introduction of standard cosmology
Dark matter evidenceDark matter evidence
New physics and dark matterNew physics and dark matter
WIMPWIMP
candidates: candidates: neutralino LSP in MSSM, lightest KK particle neutralino LSP in MSSM, lightest KK particle in UEDin UED
direct/indirect DM searches, collider studiesdirect/indirect DM searches, collider studies
synergy between cosmology and particle synergy between cosmology and particle physicsphysics
superWIMPsuperWIMP
S. Su Dark Matters 3
Standard cosmology Standard cosmology
Einstein equationsEinstein equations
MetricsMetrics
Equations of stateEquations of state
a(t): scale factora(t): scale factor
k: -1, 0, 1 for open, flat, close universek: -1, 0, 1 for open, flat, close universe
S. Su Dark Matters 4
Standard cosmology Standard cosmology
Friedmann equationFriedmann equation
Hubble Hubble parameterparameter
critical densitycritical density
S. Su Dark Matters 5
We are living through a revolution in our We are living through a revolution in our understanding of the Universe understanding of the Universe
on the largest scaleson the largest scales
For the first time in history, For the first time in history,
we have a complete picture of the Universewe have a complete picture of the Universe
S. Su Dark Matters 6
DM evidence: rotation curves DM evidence: rotation curves
NGC 2403
Rotation curves of galaxies and galactic clustersRotation curves of galaxies and galactic clusters
VVcc »» const const
VVcc »» 1/r 1/r
Dark matter Dark matter in haloin halo
Constrain Constrain mm
ii==ii//cc
S. Su Dark Matters 7
Dark matter evidence: supernovae Dark matter evidence: supernovae
SupernovaeSupernovae
Constrain Constrain mm--
S. Su Dark Matters 8
Dark matter evidence: CMB Dark matter evidence: CMB
Cosmic Microwave BackgroundCosmic Microwave Background
Constrain Constrain ++mm
thethenn
nownow
S. Su Dark Matters 9
Remarkable agreementRemarkable agreement Remarkable precision Remarkable precision (~10%)(~10%)
Synthesis Synthesis
73% 73% §§ 4% 4%
23% 23% §§ 4% 4%
3%3%
» » 0.5%0.5%
» » 0.5%0.5%
S. Su Dark Matters 11
Dark matter vs. dark energy Dark matter vs. dark energy
We know We know how muchhow much, but no idea , but no idea what it is.what it is.
Dark matterDark matter Dark energyDark energy
No known particles contributeNo known particles contribute All known particles contributeAll known particles contribute
Probably tied to mProbably tied to mweakweak »» 100 100 GeVGeV
Probably tied to mProbably tied to mPlanckPlanck »» 10 101919 GeVGeV
Several compelling solutions Several compelling solutions No compelling solutionsNo compelling solutions
S. Su Dark Matters 12
富士山富士山
Five stationFive station
Seven stationSeven station
Dark Dark EnergyEnergy
Dark Dark MatterMatter
Ordinary Ordinary mattermatter
S. Su Dark Matters 13
Standard Model Standard Model
HH
uu cc tt
dd ss bb
ee ee
WW§§,Z,Z gg
QuarksQuarks
LeptonsLeptons
Gauge bosonGauge boson(force (force carrier)carrier)HiggsHiggs
No good candidates for CDM in No good candidates for CDM in SMSM
Not for cosmology Not for cosmology observationsobservations
− Dark MatterDark Matter− Cosmology constantCosmology constant− Baryon asymmetry …Baryon asymmetry …
SM is a very successful theoretical SM is a very successful theoretical frameworkframework describes all experimental observations to describes all experimental observations to datedate
CDM CDM requirementsrequirements
Gravitational Gravitational interactinginteracting
StableStable Non-baryonicNon-baryonic NeutralNeutral Cold (massive)Cold (massive) Correct Correct densitydensity
S. Su Dark Matters 14
New physics beyond SM New physics beyond SM
DM problem provide precise, unambiguous evidence for new physicsDM problem provide precise, unambiguous evidence for new physics
Independent motivation for new physics in particle physics
New physics to protect electroweak scaleNew physics to protect electroweak scale
new symmetry: supersymmetrynew symmetry: supersymmetry new space dimension: extra-dimensionnew space dimension: extra-dimension … …
S. Su Dark Matters 15
Dark matter in new physics Dark matter in new physics
Dark Matter: new stable particleDark Matter: new stable particle
in many theories, dark matter is easier to explain than no dark matterin many theories, dark matter is easier to explain than no dark matter
there are usually many new weak scale particle there are usually many new weak scale particle constraints (proton decay, large EW constraints (proton decay, large EW corrections) corrections) discrete symmetrydiscrete symmetry
stabilitystability
good dark matter candidategood dark matter candidate
S. Su Dark Matters 16
Dark matter candidates Dark matter candidates
mass and interaction strengths span many, many orders of mass and interaction strengths span many, many orders of magnitudemagnitude
Many ideas of DM candidates:Many ideas of DM candidates:
WIMP WIMP superWIMPssuperWIMPs primodial black holesprimodial black holes
axionsaxions warm gravitinoswarm gravitinos Q ballsQ balls wimpzillaswimpzillas
self-interacting particlesself-interacting particles self-annihilating particlesself-annihilating particles fuzzy dark matterfuzzy dark matter branonsbranons … …
appear in particle physics models motivated independentlyappear in particle physics models motivated independently by attempts to solve Electroweak Symmetry Breaking by attempts to solve Electroweak Symmetry Breaking
relic density are determined by mrelic density are determined by mplpl and m and mweakweak
naturally around the observed valuenaturally around the observed value no need to introduce and adjust new energy scaleno need to introduce and adjust new energy scale
S. Su Dark Matters 17
Dark matter freeze out Dark matter freeze out
Freeze out, n/s Freeze out, n/s »» constconst
WIMPWIMP
− early time early time H H n n ¼¼ n neqeq
− late timelate time H H (n/s)(n/s)todaytoday »» (n/s) (n/s)decouplingdecoupling
− at freeze-out at freeze-out ¼¼ H H TTFF »» m/25 m/25
Approximately, Approximately, relicrelic // 1/ 1/hhvvii
=n =n hhvvii v.s. H v.s. H
ffff ff ff expansionexpansionUniverse cools: Universe cools: n=nn=nEQEQee-m/T-m/T
Boltzmann equationBoltzmann equationThermal Thermal equilibriumequilibrium
$$ ff ff
S. Su Dark Matters 18
Relic density calculations Relic density calculations
Boltzmann equationBoltzmann equation
number density at thermal number density at thermal equilibriumequilibrium
entropyentropy
S. Su Dark Matters 19
Relic density calculations Relic density calculations
Define Define
Long before freeze-Long before freeze-out out
Long after freeze-Long after freeze-out out
S. Su Dark Matters 20
Relic density calculations Relic density calculations
Approximately, relic density today ( ) Approximately, relic density today ( )
gg**: number of relativistic degrees of freedom at the time of freeze out: number of relativistic degrees of freedom at the time of freeze out
xxFF: freeze out : freeze out temperaturetemperature
g: degrees of freedom for dark g: degrees of freedom for dark matter Xmatter Xc: O(1) constant determined by matching the late-time and early-time c: O(1) constant determined by matching the late-time and early-time solutionssolutions
Or, order of magnitude estimation: Or, order of magnitude estimation:
Resonance enhancement, coannihilation …Resonance enhancement, coannihilation …
S. Su Dark Matters 21
WIMP dark matter WIMP dark matter
WIMPWIMP: Weak Interacting Massive Particle : Weak Interacting Massive Particle
mmWIMPWIMP»» m mweakweak
anan »» weakweak22 m mweakweak
-2-2
hh22 »» 0.3 0.3
naturally around the observed valuenaturally around the observed value
S. Su Dark Matters 22
SM particle superpartnerSM particle superpartner Spin differ by 1/2Spin differ by 1/2
(H(Huu++,H,Huu
00) , (H) , (Hdd00, H, Hdd
--))
uu cc tt
dd ss bb
ee ee
BB00 WW§§,W,W00 gg
SquarkSquarkss
sleptonsleptonss
GauginGauginososHiggsinHiggsinoo
»» »» »»
»»»»»»
»» »» »»
»»»»»»
»» »» »» »»
»»»»»»»»
CDM CDM requirementsrequirements
Correct Correct densitydensity
Non-baryonicNon-baryonic NeutralNeutral ColdCold
m > 45 GeVm > 45 GeV
StableStable
gravitational gravitational interactinginteracting
weak interactionweak interaction
Supersymmetry breaking, m Supersymmetry breaking, m »» TeV TeV
Minimal Supersymmetric Standard Model (MSSM) Minimal Supersymmetric Standard Model (MSSM)
S. Su Dark Matters 23
Neutralino LSP as DM Neutralino LSP as DM
new weak scale particle new weak scale particle constraints constraints discrete symmetrydiscrete symmetry
stabilitystability
dark matter candidatedark matter candidate
super-partnerssuper-partners
proton decayproton decay
R-parityR-parity: : SM particle SM particle ++ super-partner super-partner --
lightest supersymmetric particle (LSP)lightest supersymmetric particle (LSP) stablestableLSP LSP SM particle, LSP SM particle, LSP super particle super particle
BB00, W, W00, H, Hdd00, H, Huu
00
Superpartner of Superpartner of gauge bosonsgauge bosons
Superpartner of Superpartner of Higgs bosonsHiggs bosons
~~ ~~ ~~ ~~
neutralinos neutralinos ii
00, i=1…4 mass eigenstates, i=1…4 mass eigenstates
Neutralino LSP: Neutralino LSP: 1100 as Dark Matter as Dark Matter
S. Su Dark Matters 24
Sneutrino Dark Matter Sneutrino Dark Matter
~~
~~
ZZ/l/q/l/q
/l/q/l/q
~~
~~
W/ZW/Z
W/ZW/Z
~~ff
~~
~~
/l/l
/l/l
rapid annihilation, rapid annihilation, hhAAvvii large large
light sneutrino: 45-200 GeV light sneutrino: 45-200 GeV low abundance low abundance
heavy sneutrino: 550 – 2300 GeV heavy sneutrino: 550 – 2300 GeV 0.1 0.1 1 1
− disfavored on theoretical grounddisfavored on theoretical ground− excluded by nuclear recoil direct detection: mexcluded by nuclear recoil direct detection: m ¸̧ 20 TeV 20 TeV ~~
Sneutrino CDM in MSSM is disfavoredSneutrino CDM in MSSM is disfavored
S. Su Dark Matters 25
Neutralino relic density Neutralino relic density
CMSSMCMSSM
0.1 0.1 hh22 0.3 (pre-WMAP) 0.3 (pre-WMAP)
110 0
1100
ff
ff
~~ff
1100
1100
++
WW
WW
t-channelt-channel(dominate)(dominate)
absent for Babsent for B00~~
~~1100
~~1100
Z,HZ,H/l/q/l/q
/l/q/l/q
s-channels-channel
important near pole important near pole mm »» m mZ,HZ,H/2/2
Cosmology excludes Cosmology excludes much of much of the parameter spacethe parameter space
too bigtoo big
cosmology focuses cosmology focuses attention attention on particular regions on particular regions
just rightjust right
S. Su Dark Matters 26
Bulk region and coannihilation regionBulk region and coannihilation region
bulkbulk co-annihilation
co-annihilation
mm »» m m
+X +X !! +Y in +Y in equilibriumequilibrium decays into decays into eventuallyeventually
Co-annihilation:Co-annihilation:, , , ,
~~
~~~~
~~
~~
~~
mmee=99GeV=99GeV ~~
b b !! s s
Other constraintsOther constraints
− b b !! s s : : »» 10 10-4-4
exclude small mexclude small m1/21/2
important for important for <0 <0
bb ss
− muon g-2muon g-2 th-exp=(26 th-exp=(26 §§ 16) 16)££ 10 10-10-10
CMSSMCMSSM
0.1 0.1 hh22 0.3 0.3
0.094 0.094 hh22 0.129 0.129
Ellis et. al. (2003)
S. Su Dark Matters 27
Focus Point RegionFocus Point Region
conventional wisdomconventional wisdom focus pointfocus point
naturalness naturalness m m00, M, M1/21/2, |, || | TeVTeV
mm00 a few TeV , a few TeV , naturalnatural
mm00 term negligible term negligible mm00 term not negligible term not negligible
||| | ÀÀ M M11 ||| | »» M M11
DM Bino-like: DM Bino-like: 1100 ¼¼ B B00 DM Bino-Higgsino DM Bino-Higgsino
mixturemixture
(100 GeV)(100 GeV)22
~~
Feng et. al. (2000)
S. Su Dark Matters 28
Funnel-Like RegionFunnel-Like Region
~~1100
~~1100
A,HA,Hl/ql/q
l/ql/q
Large tanLarge tan : m : m »» m mA,HA,H/2/2
// 1/ 1/hhvvii
hhvvii »» 1/(4m 1/(4m22 – m – mA,HA,H
22))2 2 too bigtoo big
too smalltoo small
Ellis et. al. (2003)
S. Su Dark Matters 29
Extra dimension Extra dimension
SMSM
4D4D
Universal extra dimension: Universal extra dimension:
All SM particles live in the (flat) bulk All SM particles live in the (flat) bulk
unwanted states: orbifoldunwanted states: orbifold
Bulk field: KK towerBulk field: KK towermm22 = n/R = n/R22
……00
11
22
33
1/R1/R22
2/R2/R22
3/R3/R22
Appelquist, cheng and Dobrescu (2000)
S. Su Dark Matters 30
Universal Extra Dimension Universal Extra Dimension
new weak scale particle new weak scale particle constraints constraints
discrete symmetrydiscrete symmetry
stabilitystability
dark matter candidatedark matter candidate
KK modes of SM particleKK modes of SM particle
momentum conservation in momentum conservation in compactified dimension + compactified dimension + orbifoldingorbifolding
KK-parityKK-parity: : odd level KK odd level KK particles particles --
lightest KK state (LKP)lightest KK state (LKP) stablestable
LKP, likely to be LKP, likely to be 11stst excitation of hypercharge gauge boson B excitation of hypercharge gauge boson B(1)(1)
S. Su Dark Matters 31
UED: LKP Dark Matter UED: LKP Dark Matter
Servant, Tait (2002)
S. Su Dark Matters 32
Dark matter detection Dark matter detection
DMDM
DMDM ff
ff
// 1/ 1/hh iiNot overclose universeNot overclose universe
Efficient annihilation thenEfficient annihilation then
DM annihilationDM annihilation
Cross Cross symmetrysymmetry
DM
DM
DM
DM
ffff
DM scatteringDM scattering
Efficient scattering now Efficient scattering now directdirect DM direction DM direction
Efficient annihilation Efficient annihilation now now
indirectindirect DM direction DM direction
S. Su Dark Matters 33
Direct detection Direct detection
DMDM
detectordetector
Measure nuclear recoil energyMeasure nuclear recoil energy(ionization, photo…)(ionization, photo…)
Number of targetNumber of targetnuclei in detectornuclei in detector Local WIMP densityLocal WIMP density
(astro)(astro)
scattering cross sectionscattering cross section(particle)(particle)
S. Su Dark Matters 34
Direct detection Direct detection
WIMPWIMP
CDMCDMSS
DAMA Signal andOthers’ Exclusion Contours
CDMS (2004)
DAMADAMA
CDMS IICDMS II
CDMSCDMSEDELWEISSEDELWEISS
S. Su Dark Matters 35
Current Sensitivity
Near Future
Future
Theoretical Predictions
Bae
r, Bala
zs, Belyaev, O
’Farrill (2003)
Direct detection: future Direct detection: future
BB(1
)(1
) LK
P D
M L
KP
DM
S. Su Dark Matters 36
Indirect detectionIndirect detection
DMDMDMDM
detectordetector
Dark Matter annihilates Dark Matter annihilates
in in (amplifier) (amplifier) to to ,, a place some particles
which are detected bywhich are detected by .. an experiment
reci
pe
reci
pe
AA // n nDMDM22
S. Su Dark Matters 37
Dark Matter annihilates Dark Matter annihilates
in in center of the suncenter of the sun to to neutrinos neutrinos ,,
a place some particles
which are detected bywhich are detected by AMANDA, ICECUBEAMANDA, ICECUBE.. an experiment
reci
pe
reci
pe
earthearth
Dark matter density in Dark matter density in the sun, capture ratethe sun, capture rate
S. Su Dark Matters 38
MSSMMSSM
Indirect detection: neutrinoIndirect detection: neutrino
UEDUED
icecubeicecube
Hooper and Wang (2003) Hooper and Krib (2002)
S. Su Dark Matters 39
Dark Matter annihilates Dark Matter annihilates
in in galactic center galactic center to to photons photons ,,
a place some particles
which are detected bywhich are detected by GLAST, HESSGLAST, HESS.. an experiment re
cip
ere
cip
e
Dark matter density in Dark matter density in the center of the galaxythe center of the galaxy
HESSHESS
S. Su Dark Matters 40
MSSMMSSM
EGRETEGRET
GLASTGLAST
Indirect detection: gamma rayIndirect detection: gamma ray
UEDUED
Hooper and Wang (2003)
S. Su Dark Matters 41
Dark Matter annihilates Dark Matter annihilates
in in the halo the halo to to positions positions ,,
a place some particles
which are detected bywhich are detected by AMS on the ISSAMS on the ISS.. an experiment re
cip
ere
cip
e
Dark matter density Dark matter density profile in the haloprofile in the halo
AMSAMS
S. Su Dark Matters 42
Comparison of pre-LHC SUSY searchesComparison of pre-LHC SUSY searches
DM searches are complementary to collider searchesDM searches are complementary to collider searches
When combined, entire cosmologically attractive When combined, entire cosmologically attractive region will be explored before LHC ( region will be explored before LHC ( »» 2007 ) 2007 )
Pre-WMAPPre-WMAP
Post-WMAPPost-WMAP
LHC searchLHC search
DM searchDM search
S. Su Dark Matters 43
Collider study of dark matter Collider study of dark matter
Can study those regions at collidersCan study those regions at colliders
pppp
20072007NowNow
TevatronTevatron
pp--pp
Precise determination of new particle mass and couplingPrecise determination of new particle mass and coupling
Determine DM mass, relic densityDetermine DM mass, relic density
LHCLHC
ILCILC
S. Su Dark Matters 44
Choose four Choose four representative points for representative points for
detailed studydetailed study
Neutralino DM in mSUGRA Neutralino DM in mSUGRA
Feng et. al. ILC cosmology working group
Baer et. al. Baer et. al. ISAJETISAJETGondolo et. al. Gondolo et. al. DarkSUSYDarkSUSYBelanger et. al. Belanger et. al. MicroMEGAMicroMEGA
S. Su Dark Matters 45
Bulk region LCC1 (SPS1a) Bulk region LCC1 (SPS1a)
MM00, m, m1/21/2, A, A00, tan, tan = 100, 250, -100, 10 ( = 100, 250, -100, 10 ( >o, m>o, m3/23/2>m>mLSP LSP ))
light light 1100, , 22
00, , 11§§, slepton, slepton
Weiglein, Martyn et. al. (2004)
Scan over Scan over »» 20 20 most most relevant relevant parametersparameters
compute compute hh22, , weigh weigh each point byeach point by Gaussian Gaussian distributiondistribution for each for each observableobservable
width of pdf width of pdf hh
S. Su Dark Matters 46
WMAPWMAP(current)(current)
PlanckPlanck(~2010)(~2010)
LHC (“best case scenario”)LHC (“best case scenario”)ILCILC
LCC1
Relic density determination: LCC1 Relic density determination: LCC1
(preliminary) result: (preliminary) result: // = 2.2% ( = 2.2% ( h h22 = 0.0026 ) = 0.0026 )
Battaglia (2005)
S. Su Dark Matters 47
LCC2
Foucs point region: LCC2 Foucs point region: LCC2
(preliminary) result: (preliminary) result: // = 2.4% ( = 2.4% ( h h22 = 0.0029 ) = 0.0029 )
Battaglia (2005)
MM00, m, m1/21/2, A, A00, tan, tan =3280, 300, 0, 10 ( =3280, 300, 0, 10 ( >o, m>o, m3/23/2>m>mLSP LSP ))
light neutralino/chargino light neutralino/chargino
WMAPWMAP
PlanckPlanckILCILC
LCC2
S. Su Dark Matters 48
Coanniliation region: LCC3 Coanniliation region: LCC3
(preliminary) result: (preliminary) result: // = 7% ( = 7% ( h h22 = 0.0084 ) = 0.0084 )
Battaglia (2005)
MM00, m, m1/21/2, A, A00, tan, tan =210, 360, 0, 40 ( =210, 360, 0, 40 ( >o, m>o, m3/23/2>m>mLSP LSP ))mm »» m mstaustau
LCC3WMAPWMAP
PlanckPlanckILCILC
S. Su Dark Matters 49
Synergy Synergy
Relic Density Indirect DetectionRelic Density Indirect Detection Direct DetectionDirect Detection
Astrophysical and Cosmological InputsAstrophysical and Cosmological Inputs
Collider InputsCollider Inputs
Weak-scale ParametersWeak-scale Parameters
DM AnnihilationDM Annihilation DM-DM-NN Interaction Interaction
parts per mille parts per mille agreement for agreement for discovery discovery of dark matterof dark matter
local DM density local DM density and velocity and velocity profileprofile
eliminate particle physics eliminate particle physics uncertaintyuncertaintydo real astrophysicsdo real astrophysics
S. Su Dark Matters 50
Alternative dark matter Alternative dark matter
But the relic density argument But the relic density argument strongly prefers weak strongly prefers weak interactions.interactions.
All of the signals rely on DM having EW interactions.All of the signals rely on DM having EW interactions.
Is this required?Is this required?
CDM CDM requirementsrequirements
Gravitational Gravitational interactinginteracting (much weaker(much weaker than than electroweak)electroweak)
StableStable Non-baryonicNon-baryonic NeutralNeutral Cold (massive)Cold (massive) Correct Correct densitydensity
NO!NO!
DMDM -1-1
((gravitational gravitational coupling)coupling)-2-2
● too smalltoo small
● DMDM too big too big
overcloseoverclose the Universe the Universe
S. Su Dark Matters 51
SWIMPSWIMPSMSM
101066
superWIMP superWIMP
Feng, Rajaraman and Takayama (2003)
101044 s s t t 10 1088 s s
superWIMPsuperWIMP
e.g. Gravitino e.g. Gravitino LSPLSP LKK LKK gravitongraviton
WIMPWIMP
neutralneutral chargedcharged
WIMP WIMP superWIMP + SM particles superWIMP + SM particles
WIMPWIMP
S. Su Dark Matters 52
superWIMP : an example superWIMP : an example
SUSY caseSUSY case WIMP WIMP superWIMP + SM particles superWIMP + SM particles
Charged sleptonCharged sleptonSuperpartner of leptonSuperpartner of lepton
GravitinoGravitinoSuperpartner of gravitonSuperpartner of graviton
EM, had. cascadeEM, had. cascade
change CMB change CMB spectrumspectrum
change light change light element element
abundance predicted abundance predicted
by BBNby BBN
Strong constraints !Strong constraints !
WIMPWIMP
superWIMPsuperWIMP
SM particleSM particle
»» 11
mmplpl
Decay lifetime Decay lifetime planck mass planck mass
S. Su Dark Matters 53
Gravitino Gravitino
Gravitino: superpartner of gravitonGravitino: superpartner of graviton
Obtain mass when SUSY is spontaneously broken Obtain mass when SUSY is spontaneously broken mmGG »» F/m F/mplpl
Stable when it is LSP Stable when it is LSP - candidate of Dark Matter- candidate of Dark Matter
~~
mmG G »» m mSUSYSUSY
»» GeV – TeV GeV – TeV
coldcold Dark Matter Dark Matter
~~mmGG ¿¿ m mSUSYSUSY
» » keVkeV
warmwarm Dark Matter Dark Matter
~~
S. Su Dark Matters 54
Gravitino: warm dark matter Gravitino: warm dark matter
mmG G ¿¿ m mSUSYSUSY (GMSB)(GMSB)
~~ hh22 »» (m (mGG/keV) (100/g/keV) (100/g**))
mmGG »» keV : keV : warmwarm Dark Matter Dark Matter
mmGG keV : keV : problematic !problematic !
gravitino dilution necessarygravitino dilution necessary
stringent bounds on reheating temp. stringent bounds on reheating temp.
~~
~~
Moroi, Murayama and Yamaguchi, PLB303, 289 (1993)
~~
S. Su Dark Matters 55
Gravitino cold dark matter Gravitino cold dark matter
mmG G »» m mSUSYSUSY »» GeV – TeV GeV – TeV (supergravity)(supergravity)
~~
thermalthermalLSPLSP vv-1-1
((weak weak coupling)coupling)-2-2
GG~~
~~ ll~~ LSPLSP
WIMPWIMP
GG~~~~ ll
~~LSPLSP
superWIMPsuperWIMPDMDM
G G LSP + SM LSP + SM
BBN constraints:BBN constraints: TTRHRH 10 1055 – 10 – 1088 GeV GeV
Conflict with thermal leptogenesis:Conflict with thermal leptogenesis: TTRHRH 3 3 ££ 10 1099 GeV GeV
~~
Bolz, Brandenburg and Buchmuller,NPB 606, 518 (2001)Kawasaki, Kohri and Moroi, asrtro-ph/0402490, astro-ph/0408426
Buchmuller, Bari, Plumacher, NPB665, 445 (2003)
Kohri, Moroi and Yotsuyanagi, hep-ph/0507245
Y Y // T TRHRH
TTRHRH 10 101010 GeV GeV
S. Su Dark Matters 56
BBN constraints BBN constraints
??
Fie
lds,
Sark
ar,
PD
G (
20
02
)
Big bang nucleosynthesisBig bang nucleosynthesis
10-10 = 6.1 0.4
Late time particle decayLate time particle decay
Change light element abundanceChange light element abundance
S. Su Dark Matters 57
BBN constraints on EM/had injection BBN constraints on EM/had injection
EM,hadEM,had==EM,hadEM,had Br BrEM,hadEM,had YYNLSPNLSP
Decay lifetime Decay lifetime NLSPNLSP
EM/had energy releaseEM/had energy release
» » mmNLSPNLSP-m-mGG~~
Cyburt, Ellis, Fields and Olive, PRD 67, 103521 (2003)
EMEM
EM
(G
eV)
Kawasaki, Kohri and Moroi, astro-ph/0402490
hadhad EMEM
S. Su Dark Matters 58
Viable parameter spaceViable parameter space
slepton and sneutrinoslepton and sneutrino approach I:approach I: fix fix GG = = 0.230.23
~~
apply CMB and BBN constraints on (apply CMB and BBN constraints on (NLSPNLSP, , EM/hadEM/had ))
viable parameter spaceviable parameter space
NLSPNLSP, , EM,hadEM,had==EM,hadEM,had B BEM,hadEM,had Y YNLSPNLSP m m ·· 80 80 »» 300 GeV 300 GeV200 GeV 200 GeV ·· m m ·· 400 400 »» 1500 GeV 1500 GeV
mmGG ¸̧ 400 GeV 400 GeV~~
Feng, SS and Takayama (2004)
S. Su Dark Matters 59
superWIMP in mSUGRA superWIMP in mSUGRA
BBN EM constraints only
Stau NLSP
Ellis et. al., hep-ph/0312262
superWIMP allowed regionsuperWIMP allowed region
Usual WIMP allowed regionUsual WIMP allowed region
S. Su Dark Matters 60
Collider phenomenology Collider phenomenology
SWIMP Dark MatterSWIMP Dark Matter
no signals in direct / indirect dark matter searchesno signals in direct / indirect dark matter searches
SUSY NLSP:SUSY NLSP: rich collider phenomenologyrich collider phenomenology
NLSPNLSP in SWIMP in SWIMP: : long lifetime long lifetime stable inside the detectorstable inside the detector
Charged slepton Charged slepton highly ionizing trackhighly ionizing track
neutral WIMPneutral WIMP missing energymissing energy
S. Su Dark Matters 61
WIMP pair production:WIMP pair production: via detailed balancevia detailed balance
1/2: i,j,identical1/2: i,j,identical1: otherwise1: otherwise
relative velocity of two WIMP in CM framerelative velocity of two WIMP in CM framespinspin
Model independent DM production Model independent DM production
WIMPWIMP, , SWIMPSWIMP DMDM
WIMP annihilate efficiently in early universeWIMP annihilate efficiently in early universe
WIMP be produced efficiently at collidersWIMP be produced efficiently at colliders
Birkedal, Matchev and Perelstein, PRD70, 077701 (2004)
Upper bound on Upper bound on
Lower bound on ratesLower bound on rates
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superWIMP: Discovery limit superWIMP: Discovery limit
10 events reach10 events reach
P-waveP-waveSSXX=0=0mmSWIMPSWIMP/m/mWIMPWIMP=0.6=0.6
Scale as Scale as (2 S(2 SXX+1)+1)-2-2 and and (m(mSWIMPSWIMP/m/mWIMPWIMP))-1-1
(L=30 fb(L=30 fb-1-1)) (L=1 ab(L=1 ab-1-1))
(L=1 ab(L=1 ab-1-1), E), Ecmcm=2.8 m=2.8 mWIMPWIMP ( (=0.7)=0.7)
Signal: Signal: two isolated charged track free of hadron two isolated charged track free of hadron activityactivity
Background free !Background free !
Feng, SS and Takayama (2005)
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Neutral WIMP Neutral WIMP
WIMP pair production is invisibleWIMP pair production is invisible
Consider monojet event: eConsider monojet event: e++ee-- !! X X X X
ILC: L=500 fb-1
Birkedal, Matchev and Perelstein (2004)
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NLSPNLSP
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
SMSM
How to trap How to trap slepton?slepton?
● Decay life time Decay life time
● SM particle energy/angularSM particle energy/angular distribution …distribution … mmGG
mmplpl … …
~ ~
Probes gravity in a Probes gravity in a particle physics particle physics experiments!experiments!
BBN, CMB in the labBBN, CMB in the lab
Precise test of Precise test of supergravity: gravitino is a supergravity: gravitino is a graviton partnergraviton partner
Hamaguchi, kuno, Nakaya, Nojiri, hep-ph/0409248Feng and Smith, hep-ph/0409278
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Slepton trapping Slepton trapping
Slepton could live for a year, Slepton could live for a year, so can be trapped then moved so can be trapped then moved to a quiet environment to to a quiet environment to observe decaysobserve decays
LHC: 10LHC: 1066 slepton/yr possible, slepton/yr possible, but most are fast. but most are fast. Catch 100/yr in 1 kton waterCatch 100/yr in 1 kton water
LC: tune beam energy to LC: tune beam energy to produce slow sleptons, produce slow sleptons, can catch 1000/yr in 1 kton watercan catch 1000/yr in 1 kton water
Feng and Smith, hep-ph/0409278
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Conclusion Conclusion
We now know the composition of the We now know the composition of the UniverseUniverse
No known particle in the SM can be DMNo known particle in the SM can be DM
precise, unambiguous evidence for new precise, unambiguous evidence for new physicsphysics
New physics New physics
new stable particle as DM candidatenew stable particle as DM candidate
WIMP: neutralino LSP in MSSM, LKP in UEDWIMP: neutralino LSP in MSSM, LKP in UED
direct/indirect DM searches, collider studiesdirect/indirect DM searches, collider studies
synergy between cosmology and particle synergy between cosmology and particle physicsphysics
superWIMP: superWIMP: new viable candidate for DMnew viable candidate for DM