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.

S. Su Dark Matter 3

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

S. Su Dark Matter 4

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 …

S. Su Dark Matter 5

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

S. Su Dark Matter 6

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

S. Su Dark Matter 7

Gauge Coupling Unification Gauge Coupling Unification

SMSM

SUSYSUSY

S. Su Dark Matter 8

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

S. Su Dark Matter 9

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

~~ ~~~~~~

S. Su Dark Matter 10

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


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

~~ ~~ ~~ ~~

~~ ~~ ~~ ~~


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~~~~~~~~


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


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


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


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


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


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~~ ~~~~

~~

~~


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§§


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


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~~


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


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


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


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 )


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

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Supersymmetric Dark Matter