dark matter wimp and superwimpshufang/talk/dm_collo.pdfs. su dark matters 2-outline dark matter...

S. Su Dark Matters

Dark Matter WIMP and SuperWIMP

Shufang Su • U. of Arizona

S. Su Dark Matters 2

-

Outline

Dark matter evidence

New physics and dark matter

WIMP

candidates: neutralino LSP in MSSM

direct/indirect DM searches, collider studies

synergy between cosmology and particle physics

superWIMP


We are living through a revolution in our understanding of the Universe

on the largest scales

For the first time in history, we have a complete picture of the Universe


DM evidence: rotation curves -

NGC 2403

Rotation curves of galaxies and galactic clusters

Constrain Ωm

Ωi=ρi/ρc



NGC 2403


Vc ~ 1/r1/2Constrain Ωm

Ωi=ρi/ρc



NGC 2403


Vc ~ const

Vc ~ 1/r1/2Constrain Ωm

Ωi=ρi/ρc



NGC 2403


Vc ~ const

Vc ~ 1/r1/2

Dark matter in halo

Constrain Ωm

Ωi=ρi/ρc


Dark matter evidence: supernovae -

Supernovae

Constrain Ωm-ΩΛ


Dark matter evidence: CMB -

Cosmic Microwave Background

Constrain ΩΛ+Ωm

then now


• Remarkable agreement• Remarkable precision (~10%)

Synthesis -

Ω=73% ± 4%

Ω=23% ± 4%

Ω∼3%

Ω ~ 0.5%

Ω ~ 0.5%


Dark matter vs. dark energy -

We know how much, but no idea what it is.

Dark matter Dark energy

No known particles contribute All known particles contribute

Probably tied to mweak ~ 100 GeV Probably tied to mPlanck ~ 1019 GeV

Several compelling solutions No compelling solutions


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons

Gauge boson(force carrier)

Higgs


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs

SM is a very successful theoretical framework describes all experimental observations to date


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs

Not for cosmology observations− Dark Matter− Cosmology constant− Baryon asymmetry …


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs

CDM requirements


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs

CDM requirements

• Gravitational interacting

• Stable• Non-baryonic• Neutral• Cold (massive) • Correct density


Standard Model -

H

u c t

d s bνe

νµ ντ

e µ τ

γ W±,Z g

Quarks

Leptons


Higgs

No good candidates for CDM in SM

CDM requirements

• Gravitational interacting



New physics beyond SM -

DM problem provide precise, unambiguous evidence for new physics

Independent motivation for new physics in particle physics



SM is an effective theory below some energy scale Λ ~ TeV



Hierarchy problem




Hierarchy problem

mEW ∼102 GeV




Hierarchy problem

mplank ∼1019 GeV

mEW ∼102 GeV




Naturalness problem Hierarchy problem

mplank ∼1019 GeV

mEW ∼102 GeV




Naturalness problem

(1019 GeV)2H

∼ (100 GeV)2(mH2)physical

= (mH2)0

+ Λ2

-(1019 GeV)2

Hierarchy problem

mplank ∼1019 GeV

mEW ∼102 GeV




Naturalness problem

(1019 GeV)2H


= (mH2)0

+ Λ2

-(1019 GeV)2

Hierarchy problem

mplank ∼1019 GeV

mEW ∼102 GeVprecise cancellation up to 1034 order




New physics to protect electroweak scale• new symmetry: supersymmetry• new space dimension: extra-dimension• …

Naturalness problem

(1019 GeV)2H


= (mH2)0

+ Λ2

-(1019 GeV)2

Hierarchy problem

mplank ∼1019 GeV

mEW ∼102 GeVprecise cancellation up to 1034 order



Dark matter in new physics -

Dark Matter: new stable particle

in many theories, dark matter is easier to explain than no dark matter

• there are usually many new weak scale particle • constraints (proton decay, large EW corrections) discrete symmetry

stability

good dark matter candidate


Dark matter candidates -

mass and interaction strengths span many, many orders of magnitude

Many ideas of DM candidates:

• WIMP • superWIMPs• primodial black holes• axions• warm gravitinos• Q balls• wimpzillas

• self-interacting particles• self-annihilating particles• fuzzy dark matter• branons• …



• WIMP • superWIMPs



• WIMP • superWIMPs

• appear in particle physics models motivated independently by attempts to solve Electroweak Symmetry Breaking

• relic density are determined by mpl and mweak

− naturally around the observed value− no need to introduce and adjust new energy scale


WIMP-

Boltzmann equation

expansion χχ → ff ff → χχ


WIMP-

Boltzmann equation

WIMP

expansion χχ → ff ff → χχThermal equilibriumχχ ⇔ ff


WIMP-

Boltzmann equation


Universe cools: n=nEQ~e-m/T

WIMP


WIMP-

Boltzmann equation


Freeze out, n/s ~ const

WIMP


WIMP-

Boltzmann equation



WIMP miracle -

WIMP: Weak Interacting Massive Particle

• mWIMP~ mweak

• σan ~ αweak2 mweak

-2

⇒ Ω h2 ~ 0.3

naturally around the observed value


-

SM particle superpartner Spin differ by 1/2

(Hu+,Hu

0) , (Hd0, Hd

-)

u c t

d s b

νeνµ ντ

e µ τ

B0 W±,W0 g

Squarks

sleptons

Gauginos

Higgsino

~ ~ ~

~~~

~ ~ ~

~~~~ ~ ~ ~

~~~~

Supersymmetry breaking, m ~ TeV

Minimal Supersymmetric Standard Model (MSSM)


-


(Hu+,Hu

0) , (Hd0, Hd

-)

u c t

d s b

νeνµ ντ

e µ τ

B0 W±,W0 g

Squarks

sleptons

Gauginos

Higgsino

~ ~ ~

~~~

~ ~ ~

~~~~ ~ ~ ~

~~~~

CDM requirements

• Correct density

• Non-baryonic• Neutral• Cold

• Stable

• gravitational interacting




-


(Hu+,Hu

0) , (Hd0, Hd

-)

u c t

d s b

νeνµ ντ

e µ τ

B0 W±,W0 g

Squarks

sleptons

Gauginos

Higgsino

~ ~ ~

~~~

~ ~ ~

~~~~ ~ ~ ~

~~~~

CDM requirements

• Correct density

• Non-baryonic• Neutral• Cold m > 45 GeV

• Stable





-


(Hu+,Hu

0) , (Hd0, Hd

-)

u c t

d s b

νeνµ ντ

e µ τ

B0 W±,W0 g

Squarks

sleptons

Gauginos

Higgsino

~ ~ ~

~~~

~ ~ ~

~~~~ ~ ~ ~

~~~~

CDM requirements

• Correct density

• Non-baryonic• Neutral• Cold m > 45 GeV

• Stable


weak interaction




Neutralino LSP as DM -

• new weak scale particle • constraints discrete symmetry

stability

dark matter candidate




stability


super-partners




stability


super-partners

proton decay




stability


super-partners

proton decay

R-parity: SM particle + super-partner -




stability


super-partners

proton decay


lightest supersymmetric particle (LSP) stableLSP ⇒ SM particle, LSP ⇒ super particle




stability


super-partners

proton decay


lightest supersymmetric particle (LSP) stableLSP ⇒ SM particle, LSP ⇒ super particle

B0, W0, Hd0, Hu

0

Superpartner of gauge bosons

Superpartner of Higgs bosons

~ ~ ~ ~

⇓ neutralinos χi

0, i=1…4 mass eigenstates

Neutralino LSP: χ10 as Dark Matter


-

Neutralino relic density

CMSSM

0.1 ≤ Ωχh2 ≤ 0.3 (pre-WMAP)

• Cosmology excludes much of the parameter space

Ωχ too big

• cosmology focuses attention on particular regions

Ωχ just right


Dark matter detection -

DM

DM f

f

Ω∝1/<σv>Not overclose universe

⇓Efficient annihilation then

DM annihilation



DM

DM f

f



DM annihilation

Cross symmetry

DM

DM

ff

DM scattering



DM

DM f

f



DM annihilation

Cross symmetry

DM

DM

ff

DM scattering

Efficient scattering now direct DM direction



DM

DM f

f



DM annihilation

Cross symmetry

DM

DM

ff

DM scattering

Efficient scattering now direct DM direction

Efficient annihilation now indirect DM direction


Direct detection -

DM

detector


Direct detection -

DM

detector

Measure nuclear recoil energy


Direct detection -

DM

detector


Number of targetnuclei in detector


Direct detection -

DM

detector



Local WIMP density(astro physics)


Direct detection -

DM

detector




scattering cross section(particle physics)


Direct detection -

DM

detector




scattering cross section(particle physics)

• spin dependent scattering• spin independent scattering: dominant for heavy atom target

• elastic scattering• inelastic scattering: measure ionization, photon, …


Direct detection - 5

WIMP mass [GeV/c2]

Sp

in!

ind

epen

den

t cr

oss

sec

tion

[cm

2]

101

102

103

10!44

10!43

10!42

10!41

Baltz Gondolo 2004

Ruiz et al. 2007 95% CL


CDMS II 1T+2T Ge Reanalysis

XENON10 2007

CDMS II 2008 Ge

CDMS II Ge combined

FIG. 4: Spin-independent WIMP-nucleon cross section up-per limits (90% C.L.) versus WIMP mass. The upper curve(dash-dot) is the result of a re-analysis [17] of our previouslypublished data. The upper solid line represents the limit de-rived from our new data set. The combined CDMS limit(lower solid line) reaches the same minimum cross section asthat from Xenon10 [18] (dashed), but with more sensitivityat higher masses. Also shown are parameter ranges expectedfrom different supersymmetric models described in [19] (grey)and [20] (95% and 68% confidence levels in green and blue,respectively). Plots courtesy of [22].

(1985).

[3] B.W. Lee and S. Weinberg, Phys. Rev. Lett. 39, 165(1977); S. Weinberg, Phys. Rev. Lett. 48, 1303 (1982).

[4] G. Jungman, M. Kamionkowski, and K. Griest, Phys.Rep. 267, 195 (1996); G. Bertone, D. Hooper, and J. Silk,Phys. Rep. 405, 279 (2005).

[5] J.D. Lewin and P.F. Smith, Astropart. Phys. 6, 87(1996).

[6] E.A. Baltz, M. Battaglia, M.E. Peskin and T. Wizansky,Phys. Rev. D 74, 103521 (2006).

[7] K.D. Irwin et al., Rev. Sci. Instr. 66, 5322 (1995);T. Saab et al., AIP Proc. 605, 497 (2002).

[8] D.S. Akerib et al., (CDMS Collab.) Phys. Rev. D 72,052009 (2005).

[9] D.S. Akerib et al., (CDMS Collab.) Phys. Rev. Lett. 96,011302 (2006).


[11] CDMS Collab., in preparation.[12] A. Fasso et al., CERN-2005-10 (2005), INFN/TC 05/11,

SLAC-R-773; A. Fasso et al., arXiv:hep-ph/0306167[13] J.S. Hendricks et al., LA-UR-07-6632 available from

http://mcnpx.lanl.gov/[14] J. Allison et al., IEEE Trans. Nucl. Sc. 53 (2006) 270;

S. Agostinelli et al., Nucl. Instrum. Methods A 506(2003) 250

[15] D.S. Leonard et al., (EXO Collab.) arXiv:0709.4524v1

[physics.ins-det].[16] S. Yellin, Phys. Rev. D 66, 032005 (2002).[17] CDMS Collab., in preparation; R.W. Ogburn, Ph.D. dis-

sertation. Stanford University (unpublished).[18] J. Angle et al., (XENON Collab.) Phys. Rev. Lett. 100,

021303 (2008)[19] E.A. Baltz and P. Gondolo, JHEP 0410 (2004) 052.[20] L. Roszkowski et al. JHEP 07 (2007) 075.[21] J. Engel, Phys. Lett. B 264, 114 (1991).[22] R.J. Gaitskell, V. Mandic and J. Filippini,

http://dmtools.brown.edu

CDMS

Figure 6: Top: Improved limits on spin-dependent (pure) proton-WIMP coupling vs. WIMP

mass from this experiment (COUPP, the Chicagoland Observatory for Underground Particle

Physics). Couplings above the line would have produced signals above observed backgrounds

and are excluded to 90% C.L. Limits from other experiments are also shown (29), as well as the

(orange) region favored as a possible explanation to an existing claim for WIMP observation

(30, 31), a hypothesis now contradicted by this experiment. Bottom: Similar limits for spin-

dependent coupling parameters where no assumption is made about the relative strength of the

coupling to neutrons and protons, but a WIMP mass must be chosen (50 GeV/c2 here) (32, 33).

The region outside of the ellipses is excluded by each experiment.

19

COUPP


Direct detection - 5

WIMP mass [GeV/c2]

Sp

in!

ind

epen

den

t cr

oss

sec

tion

[cm

2]

101

102

103

10!44

10!43

10!42

10!41

Baltz Gondolo 2004



CDMS II 1T+2T Ge Reanalysis

XENON10 2007

CDMS II 2008 Ge

CDMS II Ge combined

FIG. 4: Spin-independent WIMP-nucleon cross section up-per limits (90% C.L.) versus WIMP mass. The upper curve(dash-dot) is the result of a re-analysis [17] of our previouslypublished data. The upper solid line represents the limit de-rived from our new data set. The combined CDMS limit(lower solid line) reaches the same minimum cross section asthat from Xenon10 [18] (dashed), but with more sensitivityat higher masses. Also shown are parameter ranges expectedfrom different supersymmetric models described in [19] (grey)and [20] (95% and 68% confidence levels in green and blue,respectively). Plots courtesy of [22].

(1985).

[3] B.W. Lee and S. Weinberg, Phys. Rev. Lett. 39, 165(1977); S. Weinberg, Phys. Rev. Lett. 48, 1303 (1982).

[4] G. Jungman, M. Kamionkowski, and K. Griest, Phys.Rep. 267, 195 (1996); G. Bertone, D. Hooper, and J. Silk,Phys. Rep. 405, 279 (2005).

[5] J.D. Lewin and P.F. Smith, Astropart. Phys. 6, 87(1996).

[6] E.A. Baltz, M. Battaglia, M.E. Peskin and T. Wizansky,Phys. Rev. D 74, 103521 (2006).

[7] K.D. Irwin et al., Rev. Sci. Instr. 66, 5322 (1995);T. Saab et al., AIP Proc. 605, 497 (2002).


[9] D.S. Akerib et al., (CDMS Collab.) Phys. Rev. Lett. 96,011302 (2006).


[11] CDMS Collab., in preparation.[12] A. Fasso et al., CERN-2005-10 (2005), INFN/TC 05/11,

SLAC-R-773; A. Fasso et al., arXiv:hep-ph/0306167[13] J.S. Hendricks et al., LA-UR-07-6632 available from

http://mcnpx.lanl.gov/[14] J. Allison et al., IEEE Trans. Nucl. Sc. 53 (2006) 270;

S. Agostinelli et al., Nucl. Instrum. Methods A 506(2003) 250

[15] D.S. Leonard et al., (EXO Collab.) arXiv:0709.4524v1

[physics.ins-det].[16] S. Yellin, Phys. Rev. D 66, 032005 (2002).[17] CDMS Collab., in preparation; R.W. Ogburn, Ph.D. dis-

sertation. Stanford University (unpublished).[18] J. Angle et al., (XENON Collab.) Phys. Rev. Lett. 100,

021303 (2008)[19] E.A. Baltz and P. Gondolo, JHEP 0410 (2004) 052.[20] L. Roszkowski et al. JHEP 07 (2007) 075.[21] J. Engel, Phys. Lett. B 264, 114 (1991).[22] R.J. Gaitskell, V. Mandic and J. Filippini,

http://dmtools.brown.edu

CDMS

Figure 6: Top: Improved limits on spin-dependent (pure) proton-WIMP coupling vs. WIMP

mass from this experiment (COUPP, the Chicagoland Observatory for Underground Particle

Physics). Couplings above the line would have produced signals above observed backgrounds

and are excluded to 90% C.L. Limits from other experiments are also shown (29), as well as the

(orange) region favored as a possible explanation to an existing claim for WIMP observation

(30, 31), a hypothesis now contradicted by this experiment. Bottom: Similar limits for spin-

dependent coupling parameters where no assumption is made about the relative strength of the

coupling to neutrons and protons, but a WIMP mass must be chosen (50 GeV/c2 here) (32, 33).

The region outside of the ellipses is excluded by each experiment.

19

DAMA result? COUPP


-

Indirect detection

DMDM

detector

ΓA ∝ nDM2


-

Indirect detection

DMDM

detector

Dark Matter annihilates

in (amplifier) to , a place some particles

which are detected by . an experiment

reci

peΓA ∝ nDM

2



in center of the sun to neutrinos , a place some particles

which are detected by AMANDA, ICECUBE. an experiment

reci

pe

ν

µ

earth

Dark matter density in the sun, capture rate


MSSM-

Indirect detection: neutrino

icecube

Hooper and Wang (2003)



in galactic center to photons , a place some particles

which are detected by GLAST, HESS. an experiment re

cipe

Dark matter density in the center of the galaxy

HESS


MSSM

EGRET

GLAST

-

Indirect detection: gamma ray

Hooper and Wang (2003)



in the halo to positions , a place some particles

which are detected by AMS, HEAT, PAMELA. an experiment re

cip

e

Dark matter density profile in the halo

AMS


-

Indirect detection: positron!"#$%&"'#()$%*(+,-.(/(!-0,1-((

Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02

!"#$%&'()*+$,-)./-0,)(12$'-34$%-55(3

! "#$%&'()'*%&(+*,(-.$$(/0)'

! 1%#',)#(22

Cheng, Feng, Matchev, hep-ph/0207125v2

Bringmann, astro-ph/0506219v2

e+

p-KK


-

Collider study of dark matter

Can study those regions at colliders

pp

2008Now

Tevatron

p-p

Precise determination of new particle mass and coupling⇓

Determine DM mass, relic density

LHC

ILC


Choose four representative points for detailed study

-

Neutralino DM in mSUGRA

Feng et. al. ILC cosmology working group

Baer et. al. ISAJETGondolo et. al. DarkSUSYBelanger et. al. MicroMEGA


LCC1

-

Relic density determination: LCC1

result: ΔΩχ/Ωχ = 1.0%

Battaglia (2005)


WMAP(current)

LCC1

-



Battaglia (2005)


WMAP(current)

Planck(~2010)

LCC1

-



Battaglia (2005)


WMAP(current)

Planck(~2010)

LHC (“best case scenario”)

LCC1

-



Battaglia (2005)


WMAP(current)

Planck(~2010)

LHC (“best case scenario”)ILC

LCC1

-



Battaglia (2005)


-

Comparison of pre-LHC SUSY searches

• DM searches are complementary to collider searches

• When combined, entire cosmologically attractive region will be explored before LHC ( 2008 )

Pre-WMAPPost-WMAP

LHC searchDM search


Synergy -


Synergy -

Collider Inputs

Weak-scale Parameters

DM Annihilation DM-N Interaction


Synergy -

Relic Density Indirect Detection Direct Detection

Astrophysical and Cosmological Inputs

Collider Inputs




Synergy -



Collider Inputs



parts per mille agreement for Ωχ discovery of dark matter


Synergy -



Collider Inputs




local DM density and velocity profile


Synergy -



Collider Inputs




local DM density and velocity profile

eliminate particle physics uncertaintydo real astrophysics


Alternative dark matter -

All of the signals rely on DM having EW interactions.

Is this required?




Is this required?

CDM requirements

• Gravitational interacting (much weaker than electroweak)


NO!



But the relic density argument strongly prefers weak interactions.


Is this required?

CDM requirements



NO!



But the relic density argument strongly prefers weak interactions.


Is this required?

CDM requirements



NO!

ΩDM ∝ 〈σ〉-1

∝ (gravitational coupling)-2

● 〈σ〉 too small

● ΩDM too big

overclose the Universe


superWIMP-

Feng, Rajaraman and Takayama (2003)WIMP → superWIMP + SM particles

Feng, Rajaraman, Takayama (2003);Bi, Li, Zhang (2003);Ellis, Olive, Santoso, Spanos (2003);Wang, Yang (2004);Feng, Su, Takayama (2004);Buchmuller, hamaguchi, Ratz, Yanagida (2004);Roszkowski, Ruiz de Austri, Choi (2004);Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);...


superWIMP-

Feng, Rajaraman and Takayama (2003)WIMP → superWIMP + SM particles

WIMP


superWIMP-

Feng, Rajaraman and Takayama (2003)

104 s < t < 108 s

WIMP → superWIMP + SM particles

WIMP


superWIMP-

SWIMP


104 s < t < 108 s


SM


superWIMP-


104 s < t < 108 s



superWIMP-


104 s < t < 108 s

superWIMP

e.g. Gravitino LSP LKK graviton

WIMP• neutral• charged



superWIMP in SUSY-

SUSY case WIMP → superWIMP + SM particles


superWIMP in SUSY-


Charged sleptonSuperpartner of lepton


superWIMP in SUSY-



GravitinoSuperpartner of graviton


superWIMP in SUSY-




EM, had. cascade

⇒ change CMB spectrum

⇒ change light element

abundance predicted

by BBN

Strong constraints !


superWIMP in SUSY-




EM, had. cascade

⇒ change CMB spectrum

⇒ change light element

abundance predicted

by BBN

Strong constraints !

WIMP

superWIMP

SM particle

~ 1

mpl

Decay lifetime ∝ mpl2/mG3 ~


Neutralino LSP vs. Gravitino LSP-

G~

χ,~ l~LSP

WIMP

G~

χ,~ l~

LSP

SuperWIMP


stau NLSP-

fix ΩG = 0.23~

200 GeV ≤ δm ≤ 400 ~1500 GeVmG ≤ 200 GeV~

Feng, SS and Takayama (2004)


stau NLSP-

fix ΩG = 0.23~

200 GeV ≤ δm ≤ 400 ~1500 GeVmG ≤ 200 GeV~

Feng, SS and Takayama (2004)

solve 7Li anomaly


mSUGRA-

BBN EM constraints only

Stau NLSP

Ellis et. al., hep-ph/0312262

superWIMP allowed region

Usual WIMP allowed region


-

NLSP

NLSP

NLSP

NLSP

NLSP


-

~G

~G

~G

~G

~G

SM

SM

SM

SM

SM


-

SM

SM

SM

SM

SM


-

● Decay life time

● SM particle energy/angular distribution … ⇒ mG

⇒ mpl …

~

SM

SM

SM

SM

SM


-

● Decay life time


⇒ mpl …

~

• Probes gravity in a particle physics experiments!

• BBN, CMB in the lab

• Precise test of supergravity: gravitino is a graviton partner

SM

SM

SM

SM

SM


-

How to trap slepton?

● Decay life time


⇒ mpl …

~




SM

SM

SM

SM

SM


-

How to trap slepton?

● Decay life time


⇒ mpl …

~




Hamaguchi, kuno, Nakaya, Nojiri, (2004)Feng and Smith, (2004)De Roeck et. al., (2005)

SM

SM

SM

SM

SM


slepton trapping-

Slepton could live for a year, so can be trapped then moved to a quiet environment to observe decays

Feng and Smith, hep-ph/0409278


slepton trapping-


• LHC: 106 slepton/yr possible, but most are fast. Catch 100/yr in 1 kton water



slepton trapping-


• LHC: 106 slepton/yr possible, but most are fast. Catch 100/yr in 1 kton water

• LC: tune beam energy to produce slow sleptons, can catch 1000/yr in 1 kton water



-

Conclusion


-

Conclusion We now know the composition of the Universe


-


No known particle in the SM can be DM


-



⇒ precise, unambiguous evidence for new physics


-




New physics


-




New physics

⇒ new stable particle as DM candidate


-




New physics


WIMP: neutralino LSP in MSSM, LKP in UED


-




New physics





-




New physics





superWIMP: new viable candidate for DM

dark matter wimp and superwimpshufang/talk/dm_collo.pdfs. su dark matters 2-outline dark matter...

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