Neutralino Dark Matter Yeong Gyun Kim (Korea Univ.) I.Evidence for Dark Matter II.Dark Matter Candidates III.Detection of Neutralino WIMP IV.Conclusions.

Neutralino Dark Matter

Yeong Gyun Kim(Korea Univ.)

I. Evidence for Dark MatterII. Dark Matter CandidatesIII. Detection of Neutralino WIMPIV. Conclusions

What is Dark Matter ?

: stuff that neither emits nor absorbs detectable EM radiation

: the existence can be inferred by its gravitational effects on visible celestial body

Motion of Galaxies in Clusters

Galactic Rotation Curves

Gravitational Lensing

Temperature fluctuation of CMBR ……

I. Evidence for Dark Matter

Observed the Coma cluster of galaxies in 1933:

Fritz Zwicky (1898-1974)

Motions of galaxies in clusters

Found the galaxies move too fast to be confined in the cluster by the gravitational attraction of visiblematter alone.

The central 1Mpc ofComa cluster in optical

Dark Matter in cluster

Galactic Rotation Curves

Vera Rubin (1928-)

In 1970s, they found ‘flat’ rotation curves.

Dark Matter in galaxy

Cosmic Microwave Background Anisotropies

,

,

.

Brayon

Matter

Totaletc

WMAP satellite

Matter/Energy density in the Universe

1.0Total

0.04Baryon

0.27Matter

Total Matter

Non-Baryonic Dark Matter

Dark Energy (Cosmological constant)

Matter Baryon

0.005Lumi

Baryonic Dark Matter

Baryon Lumi

( What is the Dark Matter made of ? )

MACHOs (MAssive Compact Halo Objects)

Baryonic Dark Matter candidates

; Jupiters, brown dwarfs, white dwarfs, neutron stars, black hole….

Hydrogen Gas - cold gas : 21cm line radiation - hot gas : X-ray emission …

Dusts – extinction, reddening

II. Dark Matter Candidates

Gravitaional microlensng

(EROS, MACHO)

SM neutrinos (hot DM)

Axion

Kaluza-Klein states

Non-Baryonic Dark Matter candidates

Wimpzillas (superheavy DM)

….

Lightest Supersymmetric Particle

- Neutralino- Gravitino- Axino

2 0.0076h ; WMAP + 2dFGRS(0.0005 < )

Relic density of WIMPs

Time evolution of the number density of WIMPs

H : Hubble constant

Av : thermally averaged annihilation cross section of WIMP

eqn

3T3/ 2( / 2 ) exp( / )m T m T

( )T m

( )T m

WIMP : Weakly Interacting Massive Particle

2 23 [( ) ( ) ]eqA

dnHn v n n

dt

: equilibrium number density

Freeze out atAn H

26 3 110Av cm s

2 (1)h O

2 27 3 1(3 10 / )Ah cm s v

If

Minimal Supersymmetric Standard Model (MSSM)

SM fields plus an extra Higgs doublet and their superpartners

SU(3) x SU(2) x U(1) gauge symmetry and Renormalizability

R-parity conservation (to avoid fast proton decay)

( B: baryon number, L: lepton number S: spin )

3( ) 2( 1) B L SR

= +1 for ordinary particles= -1 for their superpartners

Soft Supersymmetry Breaking

LSP is STABLE !

Neutralino mass matrix

In the basis

0 0 01 2( , , , )B W H H

1

2

0 cos sin sin sin

0 cos cos sin cos

cos sin cos cos 0

sin sin sin cos 0

Z W Z W

Z W Z W

Z W Z W

Z W Z W

M M M

M M M

M M

M M

1 2,M M : Bino, Wino mass parameters

: Higgsino mass parameter

tan

0 0 0 01 2 3 1 4 2i i i i iN B N W N H N H

: ratio of vev of the two neutral Higgs

Lightest Neutralino = LSP in many cases (WIMP !! )

Neutralino Annihilation channels

etc.

Minimal Supergravity Model

Unification of the gauge couplings at GUT scale

Universal soft breaking parameters at GUT scale

m : universal scalar mass M : universal gaugino mass A : universal trilinear coupling

Radiative EW symmetry breaking2 2 2

2 21 22

tan1

2 tan 1Z

m mM

Free parameters ( m,M,A,tan ,sgn( ) )

These conditions imply that

1 2M M at EW

scale

2M at EW scale

31 2

1 2 3 GUT

MM M M

21 2 2

5tan 0.53 WM M M

2 0.8M M

(tan 10, 0)A

Bino-like

Wino-like

0102

1 and

2 2 2 211.8 0.04

2 ZM M m

Large Am 2 2 2 21( ( ) )

2dA H Zm m EW M

Overview of the allowed regions of mSUGRA parameter space by the Relic density of Neutralino WIMP

1. Bulk region: at low m0 and m1/2: t-channel slepton exchange

2. Stau co-annihil. region: at low m0 where: neutralino-stau coannihilation

m m

3. Focus point region: at large m0 where mu is small: a sigificant higgsino comp.

,WW ZZ

4. A-annihilation region: at large tan 2Am mwhere

A ff

The Relic density of Neutralino WIMPvs.

Large Hadron Collider (LHC)

LHC : not only a discovery machine but also a precision physics tool

proton-proton at 14 TeV

10 fb^-1 integrated luminosity per year (first three years)

100 fb^-1 per year (designed)

A Case Study : Bulk region scenario

lies at low m0 and m1/2

LSP pair annihilation dominated by t-channel slepton exchange

LSP is Bino-like

The relic density of Bino LSP by t-channel right-handed slepton exchange

122 2 2 2 42

2 2 2 2 2 2 2

( )1

(1 ) ( )R

R R

e

Be e

m m m mh

TeV m m m m m

ReB

B e

e

(Drees, YGK, Nojiri, Toya, Hasuko, Kobayashi 2001)

2

2B

hbfactor

h

M

100

500

200

400

01

,Re

m m 2h measure predict

Precision measurements of sparticle masses at the LHC

When the cascade decay0 02 1Rq e is open,

a clean SUSY signal is l l + jets + missing TE events.

2q q

Re e

1e

jlm

llmjllm

(Bachacou, Hinchliffe, Paige 2000)

0 0 02 2 1

02

1/ 22 2 2 2

max2

( )( )Lq

jll

m m m mm

m

0 02 1

1/ 22 2 2 2

max2

( )( )R R

R

e e

lle

m m m mm

m

(for “point 5”, M=300 GeV and m=100 GeV)

From various end point measurement,

~ 10 % measurement of 01

,Re

m m

~ 20 % prediction of 2h

(for “point 5”, M=300 GeV and m=100 GeV)

max max max min min, , , ,jll jl ll jll jlm m m m m

: Confirmation of Neutralino DM

2 2( ) ( )h prediction h measurement

: Other DM components ?

2 2( ) ( )h prediction h measurement

: Low reheating temperature ?

Cases

2 2( ) ( )h prediction h measurement

Direct detection

30.3 /local GeV cm

270 /v km s

5 2 110010local

GeVcm s

m

Local Dark Matter density

Maxwellian velocity distribution

Local Flux of Dark Matter

III. Detection of Neutralino WIMP

Principles of WIMP detection

• Elastic scattering of a WIMP on a nucleus inside a detector

310v c

• The recoil energy of a nucleus with mass2

22

(max) 2( )recoil x N

N

mE v m

m m

610 10recoil NE m keV For

• This recoil can be detected in some ways :

Electric charges released (ionization detector)

Flashes of light produced (scintillation detector)

Vibrations produced (phonon detector)

Nm

Low energy effective Lagrangian for neutralino-quark int.

scalar interaction

5 5( ) ( ) ( ) ( ) ....q qL f qq d q q

spin-dep. interaction

• The other terms are velocity-dependent contributions and can be neglected in the non-relativistic limit for the direct detection.

• The axial vector currents are proportional to spin operatorsin the non-relativistic limit.

2 2 232( 1)spin F rG m J J

1( )p p n na S a S

J

( , ),

, , 2q p n

p n qq u d s F

da

G

( , )p nq : the quark spin content of the nucleon

Spin-dep. Neutralino-Neucleus cross-section

2

2 2313 142

...8

qq

W

g Td N N

M

,p nS

where (J : the spin of the nucleus)

: the expectation values of the spin content of the nucleus: depends on the target nucleus

( ) 0.78,pu ( ) 0.48,p

d ( ) 0.15ps

, 0.011,0.491p nS for 73Ge

, 0.415, 0.047p nS for19F

Nr

N

m mm

m m

: reduced mass

224( )scalar r p nm Zf A Z f

, ( , ) ( , )

, , , ,,

2

27p n q qp n p n

Tq TGq u d s q c b tp n q q

f f ff f

m m m

Scalar Neutralino-Neucleus cross-section

2( )

12 11 13 142

cos 1Re ( tan )( cos sin )

4 cosH d

d WW H

g mf N N N N

m m

where

( ) 0.020,pTuf

A : the atomic weight, Z : the nuclear electric charge

( , ), , | | , ,p np n Tq qm f p n m qq p n ( , ) ( , )

, ,

1p n p nTG Tq

q u d s

f f

( ) 0.026,p

Tdf ( ) 0.118pTsf

( ) 0.014,nTuf

( ) 0.036,nTdf ( ) 0.118n

Tsf

• In most instances, p nf f

2 2 24scalar r pm A f

: the scalar (spin-independent) cross section scales with the atomic weight, in contrast to the spin-dependent cross section.

• The scalar interaction almost always dominates for nuclei with A > 30.

: For , either interaction can dominate, depending on the SUSY parameters.

: has predominantly spin-independent interactions.

19F

73Ge

scalar spinvs.

mSUGRA model ( A=0 and m,M < 1TeV )

Higgs and sparticle masses and ( )B b s

bounds included.

Required that Neutralino is LSP

tan 55

7( ) 3.8 10sB B •

(S.Baek, YGK, P.Ko 2004 )

Scalar cross section of Neutralino-proton scattering

Non-universal Higgs mass Model (NUHM)

Parameterize the non-universality in the Higgs sector at GUT scale

2 21(1 ),

dHm m 2 2

2(1 )uH

m m

The above modifications of mSUGRA boundary cond. lead to the change of and at EW scale. Am

2 2 21( )

2uH Zm EW M

2 2 2 2( ) ( ) 2d uA H Hm m EW m EW

2 2 21( )

2dH Zm EW M

tan 35, 0A mSUGRA NUHM 1 2( 1, 1)

tan 35, 0A mSUGRA NUHM 1 2( 1, 1)

Non-Universal Higgs Mass Model 1 2( 1, 1)

tan 35, 0A

6( ) 3.8 10sB B •

•

7( ) 3.8 10sB B •

Non-Universal Higgs Mass Model 1 2( 1, 1)

tan 50, 0A

6( ) 3.8 10sB B •

•

7( ) 3.8 10sB B •

A specific D-brane Model

the SM gauge groups and 3 generations live on different Dp branes.

In this model, scalar masses are not completely universal and gaugino mass unificaion can be relaxed.

the string scale is around GeV rather than GUT scale.1210

Free parameters:3/ 2 1,2tan , , , ,sgn( )m

3/ 2 1 ,m TeV 0 2 , 1,21 1

A D-brane Modeltan 50

Indirect detection of Neutralino WIMP (neutrino telescopes : SuperK, Amanda, Antares, IceCube …)

Neutralino in the galactic halo can be captured into SUN (or Earth) by Neutralino-nucleus scattering

The neutrinos can be detected via conversion in neutrino telescope

The accumulated Neutralinos annihilate into SM particles, which ultimately yields energetic neutrino flux

The muon flux strongly depends on Neutralino-nucleus scattering

Muon Flux vs. mmSUGRA model ( A=0 and m,M < 1TeV )

from the Sun from the Earth

tan 55 tan 55

(S.Baek, YGK, P.Ko PRELIMINARY)

Muon Flux vs. mNon-Universal Higgs Mass Model

from the Sun from the Earth

(S.Baek, YGK, P.Ko PRELIMINARY)

Muon Flux vs. mNon-Universal Higgs Mass Model

from the Sun from the Earth

(S.Baek, YGK, P.Ko PRELIMINARY)

Muon Flux vs. mA D-brane Model

tan 55

(S.Baek, YGK, P.Ko PRELIMINARY)

tan 50

from the Earthfrom the Sun

tan 50

IV. Conclusion

Backup Slides

Acoustic Peak Region, (90 < l < 900): described by the physics of photon-baryon fluid responding to

fluctuation in the gravitational potential produced by the Dark Matter.

The Position of the First Peak Geometry of the universe.

The Amplitude of the First Peak

depends on Omega_b h^2, Omega_m h^2

Increasing O_m h^2 decreases the peak height. (reducing the effects of “radiation driving”)

The Amplitude of the Second Peak Increasing omega_b h^2 decreases its height (increasing the inertia in the photon-baryon fluid) Increasing n_s increases the height of the peak relative to the first.

The Amplitude of the Third Peak Measuring the third peak helps mostly in measuring n_s. ( long l base line makes the ratio to the first peak sensitive to n_s)

Age of the universe in a flat geometry

If the LSP is bino-like, slepton masses are moderate and one is far away from s-channel poles,

the LSP mass density is essentially determined by t-channel right-handed slepton exchange.

1. A pure bino couples only to fermion and sfermion, or Higgs and higgsino. Higgsino exchange is suppressed for

2.

2 2M

R Le e qm m m m in mSUGRA,

therefore right-handed slepton exchange is least suppressed by large mass in the propagator.

3. The hypercharges of sleptons satisfy the relation 2R Le eY Y

therefore ( ) 16 ( )R Le v e v when sfermion masses are equal.

III. sB decays in MSSM

In the Standard Model

• the decay proceeds through Z penguin and W exchange box diagrams.

• the decay is helicity suppressed due to angular momentum conservation.

9( ) 3 10SM sB B

Current Experimental Limit (90% CL)

7exp ( ) 5.8 10sB B

73.8 10

(CDF)

(D0, FPCP04)

In the MSSM (Babu,Kolda 2000)

• Fermion mass eigenstates can be different from the Higgs interaction eigenstates.

• This generates Higgs-mediated FCNCs.

3tan

21/ Am

p vs. ( )sB B

Both observables increase as tan increases.

Smaller Higgs masses give larger observable values.

2tanp

6( ) tansB B

41/p Am

4( ) 1/s AB B m

Experimental Results

(Munoz, hep-ph/0309346)

mSUGRA model ( A=0 and m,M < 1TeV )

Higgs and sparticle mass and ( )B b s

bounds included.

2 0.095h •

• 20.095 0.13h

• 2 0.13h

Non-Universal Higgs Mass Model 1 2( 1, 1)

tan 35, 0A

Non-Universal Higgs Mass Model 1 2( 1, 1)

tan 50, 0A

Non-Universal Higgs Mass Model 1 2( 1, 1)

tan 50, 0A

Non-Universal Higgs Mass Model 1 2( 0, 1)

tan 35, 0A

Non-Universal Higgs Mass Model 1 2( 0, 1)

tan 50, 0A

A D-brane Modeltan 50

Muon Flux from the SUN vs. p

Muon Flux from the SUN vs. ( )sB B

Muon Flux from the SUN vs. m

V. Conclusions

We investigated the correlation between scalar cross section for neutralino-proton scattering and branching ratio of decaysin mSUGRA, Non-Univ. Higgs mass and a D-brane model.

Both observables increase as increase and decrease.

Therefore, we find a positive correlation between two observables, though the detailed predictions differ between models.

sB

tan Am

Current upper limit on the branching ratio already puts strong constraint on the model parameter space which could lead toquite large neutralino-proton scattering cross section.

sB