Download - Supersymmetric Dark Matter
Supersymmetric Dark Matter Supersymmetric Dark Matter
Shufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of Arizona
K. Olive, astro-ph/0301505
S. Su Dark Matter 2
Composition of the Universe Composition of the Universe
»» 0.7 0.7
Dark EnergyDark Energy, quintenssence,…, quintenssence,…
»» 0.02 baryon 0.02 baryon
0.1 - 0.30.1 - 0.3Non-baryonic Non-baryonic dark matterdark matter
Baryonic dark matter (Baryonic dark matter (lumlum»» 0.003) 0.003)
Hot dark matter: NeutrinoHot dark matter: Neutrino Cold dark matterCold dark matter
− WIMPWIMP− axions axions
Other possibilitiesOther possibilities− self-annihilating DMself-annihilating DM− self-interacting DMself-interacting DM− warm DMwarm DM− fuzzy CDMfuzzy CDM− … …
We know We know how muchhow much, but no idea , but no idea what it is.what it is.
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WIMP CDM WIMP CDM
requirementsrequirements
StableStable− lifetime lifetime ¸̧ 10 Gyr 10 Gyr
Non-baryonicNon-baryonic Neutral:Neutral: color color (strong interaction)(strong interaction) and electric and electric
− strong upper limits on the abundance of strong upper limits on the abundance of anomalouslyanomalously heavy isotopesheavy isotopes
Cold: Cold: non-relativisticnon-relativistic
Yield correct density Yield correct density WIMP WIMP − weak interacting: weak interacting: »» 0.01, m 0.01, mWW »» 100 GeV 100 GeV
»» 0.1 0.1
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Standard Model Standard Model
HH
uu cc tt
dd ss bb
ee
ee
WW§§,Z,Z gg
II IIII IIIIII
QuarksQuarks
LeptonsLeptons
Gauge bosonGauge boson(force (force carrier)carrier)
HiggsHiggs
electroelectro
--magnetimagneticc
»» 0.01 0.01
weakweak
»» 0.03 0.03
strongstrong
»» 0.1 0.1
=g=g22/4/4
SM is a very successful SM is a very successful theoretical framework that theoretical framework that describes all experimental describes all experimental observations to dateobservations to date
Not for cosmology observationsNot for cosmology observations− Dark MatterDark Matter− Cosmology constantCosmology constant− Baryon asymmetry …Baryon asymmetry …
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Standard Model Standard Model
HH
uu cc tt
dd ss bb
ee
ee
WW§§,Z,Z gg
II IIII IIIIII
QuarksQuarks
LeptonsLeptons
Gauge bosonGauge boson(force (force carrier)carrier)HiggsHiggs
CDM CDM requirementsrequirements
Correct densityCorrect density
StableStable Non-baryonicNon-baryonic NeutralNeutral ColdCold
No good candidates for CDM in No good candidates for CDM in SMSM
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Supersymmetry Supersymmetry
SM is an effective theory below some energy scale SM is an effective theory below some energy scale
Hierarchy problem:Hierarchy problem: MMEWEW100 GeV , M100 GeV , Mplankplank 10101919 GeV ? GeV ? Naturalness problem:Naturalness problem: mass of a fundamental scalar mass of a fundamental scalar (like (like Higgs) receive Higgs) receive huge huge quantum corrections: quantum corrections:
(m(mHH22))physicalphysical (m (mHH
22))0 0 + + 22 (100 GeV)(100 GeV)22
-(10-(101919 GeV) GeV)22precise cancellation precise cancellation up to 10up to 1034 34 orderorder
SupersymmetrySupersymmetry SM particle superpartnerSM particle superpartner Spin differ by 1/2Spin differ by 1/2
(10(101919 GeV) GeV)22
HH
- - 22
HH
Naturalness Naturalness m ms-particles-particle »» O(100-1000) GeV O(100-1000) GeV
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Gauge Coupling Unification Gauge Coupling Unification
SMSM
SUSYSUSY
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SM particle superpartnerSM particle superpartner Spin differ by 1/2Spin differ by 1/2
Minimal Supersymmetric Standard Model (MSSM)
Minimal Supersymmetric Standard Model (MSSM)
(H(Huu++,H,Huu
00) , (H) , (Hdd00, H, Hdd
--))
uu cc tt
dd ss bb
ee
ee
BB00 WW§§,W,W00 gg
SquarksSquarks
sleptonssleptons
GauginosGauginos
HiggsinoHiggsino
CDM CDM requirementsrequirements
Correct Correct densitydensity
StableStable Non-baryonicNon-baryonic NeutralNeutral ColdCold
»» »» »»
»»»»»»
»» »» »»
»»»»»»
»» »» »» »»
»»»»»»»»
m > 45 GeVm > 45 GeV
weak interactionweak interaction
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MSSM DM Candidates MSSM DM Candidates
General MSSM, including B,L-violating operatorsGeneral MSSM, including B,L-violating operators
• dangerous dangerous introduce proton decay introduce proton decay p p !! K K++
• R-parity R-parity SM particle:SM particle: even even + + superparticle: superparticle: odd odd --− no proton decayno proton decay− lightest supersymmetric particle (LSP) lightest supersymmetric particle (LSP) stablestable LSP LSP SM particle, LSP SM particle, LSP super particle super particle Good candidate of DM: could be Good candidate of DM: could be or or 11
00
Possible DM candidatesPossible DM candidates− sneutrino sneutrino − neutralino (Bneutralino (B00,W,W00,H,Hdd
00,H,Huu00) ) !! ii
00 Stable Stable ??
dd
uuuu uu
PPKK++
~~ss--
ss--
----
~~
~~
oddodd oddodd
~~ ~~~~~~
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Sneutrino Dark Matter Sneutrino Dark Matter
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
~~
~~
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
~~
Sneutrino CDM in MSSM is excludedSneutrino CDM in MSSM is excluded
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Neutralino Neutralino
BB00, W, W00, H, Hdd00, H, Huu
00
PropertiesProperties− fermion fermion − neutralneutral− heavy: heavy: m > 45 GeVm > 45 GeV
(B(B00, W, W00, H, Hdd00, H, Huu
00) ) neutralinos neutralinos ii00, i=1…4 mass eigenstates, i=1…4 mass eigenstates
Interactions: Interactions: weak interacting weak interacting // gauge coupling gauge coupling
Superpartner of Superpartner of gauge bosonsgauge bosons
Superpartner of Superpartner of Higgs bosonsHiggs bosons
ff
ff
~~
HH
W,ZW,Z
~~ ~~ ~~ ~~
~~ ~~ ~~ ~~
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Lightest Neutralino CDM Lightest Neutralino CDM
Now let us focus on neutralino as a candidate for CDMNow let us focus on neutralino as a candidate for CDM
Neutralino mass matrixNeutralino mass matrix
Input parameter: MInput parameter: M11, M, M22, , , tan, tan
For small mixing: mFor small mixing: mZZ ¿¿ M M11, M, M22, ,
MM11< M< M22, |, ||: B|: B00 Bino-LSP Bino-LSPMM22< M< M11, |, ||: W|: W00 Wino-LSPWino-LSP|||< M|< M11, M, M22: H: Huu
00 §§ H Hdd0 0 Higgsino-LSPHiggsino-LSP
~~~~
~~
~~
ii00==ii B B00+ + ii W W00++ii H Hdd
00 + +ii H Huu00 , m , m11 m m2 2 mm3 3 m m44 , , 11 being LSP being LSP~~~~~~~~
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MSSM Parameters MSSM Parameters
Interactions involve the whole set of MSSM parameters Interactions involve the whole set of MSSM parameters > 100 new parameters > 100 new parameters (SM: 19 parameters)(SM: 19 parameters) other experimental constraintsother experimental constraints
Simplest assumption (unification)Simplest assumption (unification)
mm00 MM1/21/2 AA00 tantan sign sign
GUT scaleGUT scale
|||,b replaced by m|,b replaced by mZZ, tan, tan
common scalar common scalar mass mass common gaugino common gaugino mass mass common trilinear common trilinear scalarscalar
Low Low energy energy MSSM MSSM parameterparameterss
CMSSM CMSSM (constrained MSSM)(constrained MSSM)
LSPLSP
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Relic Density Relic Density
Thermal relic densityThermal relic density
− early timeearly time n n ¼¼ n neqeq
− late timelate time (n/s)(n/s)todaytoday »» (n/s) (n/s)decouplingdecoupling
− at freeze-outat freeze-out T T »» m/20 m/20
Decoupling: Decoupling: =n=nhhvvii ¼¼ H H
n/s
n/s
Approximately, Approximately, relicrelic // 1/ 1/hhvvii
!! X+Y X+Y>H>H
<H<H
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Neutralino Relic Density (I)Neutralino Relic Density (I)
~~1100
~~1100
Z,HZ,H /l/q/l/q
/l/q/l/q
110 0
1100
ff
ff
~~ff
1100
1100
++
WW
WW
t-channelt-channel(dominate)(dominate)
s-channels-channel Important near poleImportant near polemm »» m mZ,HZ,H/2/2
absent for Babsent for B00~~
Relic Density:Relic Density: ==hhAAvvii n n »» H H
− Co-annihilation:Co-annihilation: mmLSPLSP ¼¼ m mNLSPNLSP − Annihilation near a pole: Annihilation near a pole: e.g.e.g. mm »» m mZ,HZ,H/2/2
Special cases: Special cases: <<v> = a+bx+…v> = a+bx+…x=T/mx=T/m
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Neutralino Relic Density (II)Neutralino Relic Density (II)
bulkbulk
mm
»»
m mA.H
A.H/2/2Focus p
oint
Focus p
oint
mm=
m=
mZ
,hZ
,h/2/2
stau LSPstau LSP
No EWSBNo EWSB0.1 0.1 hh22 0.3 0.3
Co-annihilation
Co-annihilation 1100 -l-l ~~
CMSSMCMSSM
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Phenomenological ConstraintsPhenomenological Constraints
Other constraintsOther constraints− Higgs massHiggs mass mmhh > 114.4 GeV > 114.4 GeV− b b !! s s : : »» 10 10-4-4
exclude small mexclude small m1/21/2
important for important for <0 <0
− muon g-2muon g-2 th-exp=(26 th-exp=(26 §§ 16) 16)££ 10 10-10-10
bb ss
b b !! s s
muon g-2muon g-2
mmee=99GeV=99GeV~~
mm= m= mZ,hZ,h/2 region /2 region already excluded already excluded
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Bulk region and -l coannihilation regionBulk region and -l coannihilation region
if ignore co-annihilationif ignore co-annihilation
hhvvii »» 1/m 1/m22, , // m m//hhvvii
upper bound on mupper bound on m
mmhh
mmBB »» 200 GeV 200 GeV~~
~~
bulkbulk
mm »» m m
+X +X !! +Y in +Y in equilibriumequilibrium decays into decays into eventuallyeventually
Co-annihilation:Co-annihilation:, , , ,
~~
co-annihilatio
n
co-annihilatio
n~~ ~~~~
~~
~~
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Funnel-Like RegionFunnel-Like Region
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
~~1100
~~1100
A,HA,H /l/q/l/q
/l/q/l/qA,H: heavy HiggsesA,H: heavy HiggsesSM: SM: h h00
MSSM: hMSSM: h00,H,H00,A,H,A,H§§
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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
~~
Co-annihilation, funnel and focus point regions are very fine-tunedCo-annihilation, funnel and focus point regions are very fine-tunedHighly depend on the other input parametersHighly depend on the other input parameters
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Direct Detection of DMDirect Detection of DM
− Bino DM: no diagram 1Bino DM: no diagram 1 require small mrequire small m00
− Bino-Higgsino DMBino-Higgsino DM large mlarge m00 detectable detectable
Direct detection via neutralino-nucleon scatteringDirect detection via neutralino-nucleon scattering
DM low velocity, non-relativisticDM low velocity, non-relativistic− Spin-dependent:Spin-dependent: ii q q ii q q MMspinspin // pp
qq hh S Sppii/ J/ JNN + + nnqq hh S Snnii/ J/ JNN
− Spin-independent:Spin-independent: q m q mqq q / m q / mWW
MMscalarscalar // Z f Z fpp+ (A-Z) f+ (A-Z) fnn
--
--
,Z
// 1/m 1/mqq22~~
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Neutralino-Nucleon Scattering (II)Neutralino-Nucleon Scattering (II)
2 2 ££ 10 10-10-10 pb pb SISI 6 6 ££ 10 10-8-8 pb pb2 2 ££ 10 10-7-7 pb pb SDSD 10 10-5-5 pb pb
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DAMA and CDMSDAMA and CDMS
• DAMA finds signal DAMA finds signal in annual modulation in annual modulation as earth passes as earth passes through WIMP windthrough WIMP wind
• CDMS CDMS andand Edelweiss Edelweiss excludes excludes much of the favored much of the favored regionregionCMSSMCMSSM
NUHMNUHMNUHMNUHM
DAMADAMA CDMSCDMS
EdelweissEdelweiss
pb = 10pb = 10-36-36 cm cm22
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Indirect DetectionIndirect Detection
DM annihilation products from the Sun, Earth, galaxyDM annihilation products from the Sun, Earth, galaxy
require require hardhard annihilation products annihilation products (not good for Bino DM)(not good for Bino DM)
from the core of the Earth and Sunfrom the core of the Earth and Sun
ee++ from the local solar neighborhood from the local solar neighborhood
from the Galactic centerfrom the Galactic center
Atmospheric Cherenkov telescopes, space-based Atmospheric Cherenkov telescopes, space-based ray detectors ray detectors
Anti-matter/ anti-particle experimentsAnti-matter/ anti-particle experiments
Under-ice, underwater neutrino telescopesUnder-ice, underwater neutrino telescopes
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Comparison of pre-LHC SUSY SearchesComparison of pre-LHC SUSY Searches
− DM searches are complementary to collider DM searches are complementary to collider searchessearches− When combined, entire cosmologically When combined, entire cosmologically attractive region will be explored before LHC ( attractive region will be explored before LHC ( »» 2007 )2007 )
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ConclusionConclusion
DM is the one of the strongest DM is the one of the strongest phenomenologicalphenomenological motivation for new physicsmotivation for new physics
Fruitful interplay of particle physics, Fruitful interplay of particle physics, cosmology, cosmology, and astrophysicsand astrophysics
A fascinating time: we know A fascinating time: we know how muchhow much, , but have no idea but have no idea what what it isit is
Many, many experimentsMany, many experiments
MSSM neutralino LSP is a good candidate MSSM neutralino LSP is a good candidate for CDMfor CDM
In SUSY, DM searches are promising, highlyIn SUSY, DM searches are promising, highly complementarycomplementary to collider searches to collider searches