jose a.r. cembranos et al- collider signatures of superwimp warm dark matter

8/3/2019 Jose A.R. Cembranos et al- Collider Signatures of SuperWIMP Warm Dark Matter

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Jose A. R.Jose A. R. CembranosCembranos

Dept. of Physics and AstronomyDept. of Physics and AstronomyUniversity of California, IrvineUniversity of California, Irvine

IrvineIrvine , CA 92697, CA 92697

Collaborators:Collaborators: James S. Bullock,James S. Bullock,

Jonathan L.Jonathan L. FengFeng ,, ManojManoj KaplinghatKaplinghat ,,ArvindArvind RajaramanRajaraman , Bryan T. Smith, Bryan T. Smith

andand FumihiroFumihiro TakayamaTakayama

ColliderCollider Signatures ofSignatures ofSuperWIMPSuperWIMP Warm Dark MatterWarm Dark Matter


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Snowmass 2005 J.A.R. Cembranos 1

CONTENTSCONTENTS1.- Dark Matter

2.- Motivation

3.- A new signal

2.a. Theoretical2.b. Experimental

Candidates beyond SM

3.a. Small scale structure

3.b. Collider implications

SuperWIMPs WIMPsvs

Known signals and constraints:2.b.1. Big Bang nucleosynthesis2.b.2. Cosmic microwave background

2.b.3. Cosmic ray production


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DARK MATTER EVIDENCESDARK MATTER EVIDENCES

4.- Nucleosynthesis

3.- Large ScaleStructures (LSS)

DARK HALO1.- Rotation curves

2.- Cosmic Microwave Background


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EnergyEnergy ContentContent

ofof thethe UniverseUniverse

73%

23%4%

Dark Energy

Non Barionic Cold Dark Matter

Standard Model Matter

BaryonicBaryonic

COSMOLOGICAL MODELCOSMOLOGICAL MODEL

Search of DM candidates beyond the SM.

T h e S t a n d a r d C o s m

o l o g y w a n t s

n o n S t a n d a r d P a r t i

c l e s


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Among the most well-motivated candidates are theweakly-interacting massive particles (WIMPs) withmasses of the order of the weak scale M ~ 100 GeV:

DARK MATTER CANDIDATESDARK MATTER CANDIDATES

1.- Supersymmetric (SUSY) models :Lightest supersymmetric particle (LSP): Neutralinos,

WIMPS behave as cold DM (CDM) and are remarkablysuccessful in explaining the observed large scale

structure down to length scales of ~ 1 Mpc.

2.- Universal Extra Dimensions (UED):Lightest KK mode (LKKM): B 1,

3.- Brane-World Scenarios (WBS):Branons,


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Superweakly-interacting massive particles(SWIMPs) appear naturally in the same wellmotivated scenarios:

SUPERWIMP MODELSSUPERWIMP MODELS

1.- Supersymmetric (SUSY) models :Lightest supersymmetric particle (LSP): gravitinos,axinos, quintessinos

The relic density of SuperWIMPS also yieldsto the observed dark matter abundance sincethey are produced by the decay of a typicalWIMP.

2.- Universal Extra Dimensions (UED):

Lightest KK mode particle (LKKM): G 1,


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Freeze out

Increasing

C o m o v i n g N u m b e r D e n

s i t y

Increasing < sA v> < sA v>2. Decay

WIMPsWIMPs vs.vs. SuperWIMPsSuperWIMPsThe evolution of the WIMP number density follows the Boltzmann

equation:

Thermal equilibrium density:

n WIMP eq = g/(2 )3 f(p) d 3pWhen = n WIMP < H , the

DM is frozen out.

dn WIMP /dt = -3Hn WIMP - < Av >[(n WIMP )2- (n WIMP eq )2]

WIMP relic density:WIMP h 2 m WIMP / AvWIMPTFreeze out ~ m WIMP / 20

SWIMP relic density:SWIMP h 2 = WIMP h 2 m SWIMP /m WIMP

m SWIMP / AvWIMP

1. Freeze out

Increasing < v>< sA v> < sA v>

( Time )


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A. Belyaev, ALCPG, Snowmass (2005)

MSUGRA PARAMETER SPACEMSUGRA PARAMETER SPACE

{ m 0, M 1/2 , A 0, tan , sgn( ) , m 3/2 }

1.c. LSP

h2 > 0.13 excluded

1.a. LSP excluded

For example, mSUGRA have 6 free parameters:

1.- WIMP scenario:

1.b. LSP favored

2.c. NLSP h2 > 0.13 favored

2.a. NLSP favored2.- SuperWIMP scenario:

2.b. NLSP disfavored

Complementary scenarios


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1.- Big Bang nucleosynthesis

SIGNALS AND COSTRAINTSSIGNALS AND COSTRAINTS

Late decays modify late elements abundances.They can reduce the 7Li and explain the presentinconsistent measurements ( ).

3.- Cosmic rays

The superWIMP signatures are completely different tothe typical WIMP signals:

Feng et al. , PRD 68, 063504 (2003)

The same analyses constraint superWIMPmodels: NLSP disfavored.

2.- Cosmic microwave backgroundLate decays may also distort the CMB spectrum,from the Planck spectrum ( =0) to

a general Bose-Einstein one.

Sleptons NLSP are produced in cosmic rays and could be detected:1.- With high energy neutrino telescopes (IceCube,)

2.- With sea water analyses since the staus are trapped in Earth.Albuquerque

et al., PRL 92, 221802 (2003) X. Bi

et al., PRD 70, 123512 (2004) Cembranos et al. , in progress

Cyburt et al. , PRD 67, 103521 (2002)

Feng et al. , PRD 70, 063514 (2004)


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CDM appears to face difficulty in explaining the observedstructure on length scales < 1 Mpc.

SMALL SCALE PROBLEMSSMALL SCALE PROBLEMS

1.- Overdense cores in galactic halos

2.- Too many dwarf galaxies in the local Group3.- Disk galaxies with angular momentum loss.

Superweakly-interacting massive particles (SuperWIMPsor SWIMPs) can resolve these problems since they areproduced with large velocities at late times.Consequently:

A.- Reduce the phase space density smoothingout cusps in DM halos.B.- Damp the linear power spectrum reducing

power on small scales.


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1.- The velocity or angular momentum of DM halos can beincreased in the SWIMP scenario

STRUCTURE FORMATIONSTRUCTURE FORMATION

1.a. Reducing the phase space density

2.- Small scales in the linear Power Spectrum are damped:2.a Free-streaming scale 2.b. Acoustic damping scale

M. Kaplinghat, astro-ph/0507300 Sigurdson and Kamionkowski, PRL 92, 171302 (2004)

Cembranos et al. hep-ph/0507150


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GRAVITINO AND AXINO STUDIESGRAVITINO AND AXINO STUDIES

Preferred regions for Q and FS with a slepton as NLSPA. Gravitino B. Axino

=

Brandenburg et al. , PLB 617, 99 (2005)

Feng et al. , PRL 91, 011302 (2003)


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1.- CHARGED NLSP

Production of two metastable sleptons

Highly ionizing charged tracks

COLLIDER SIGNATURESCOLLIDER SIGNATURES

2.- Neutral NLSPNew motivations to distinguish between the

neutralino and sneutrino NLSP models

Feng and Smith, PRD 71, 015004 (2005)

Hamaguchi et al. , PRD 70, 115007 (2004)


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TRAPPING SLEPTONSTRAPPING SLEPTONS1.- Sleptons are missed in theenvironment of the detector.



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TRAPPING SLEPTONSTRAPPING SLEPTONS

2.- Slepton are trapped in tanks of

water.

1.- Sleptons are missed in theenvironment of the detector.



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TRAPPING SLEPTONSTRAPPING SLEPTONS

Quiet Environment

4.- We wait for detecting thedecays.

A.- In the LHC, the trap cancatch ~100/yr in 100m3we If it produces

around 10 6 sleptons/yr.

2.- Slepton are trapped in tanks of

water.

1.- Sleptons are missed in theenvironment of the detector.

3.- The water is moved to a quietenvironment.

Collider

B.- By tuning the beamenergy in the ILC to

produce slow sleptons, itis possible to trap ~100/yrin 100 m 3we.



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The lower areas areaccessible at futurecollider experiments(LEP-II fixes the presentexclusion region) .

COLLIDER SENSITIVITIESCOLLIDER SENSITIVITIESA. Gravitino B. Axino


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CONCLUSIONSCONCLUSIONS

1.- We have examined the implications of superWIMP(SWIMP) dark matter (DM) for small scale structures.

3.- These analyses could be interpreted as a new SWIMP signal or as anew SWIMP constraint depending of future astrophysical observations.

2.- Because SWIMPs are produced with large velocity in late decays,

their behavior in relation with structure formation can differ verymuch of cold DM.

4.- We have analyzed the consequences for collider experimentssupposing pure SWIMP DM scenarios:

4.a. In the gravitino SWIMP case, no signal is expected in the ILC.The LHC only will be sensitivity to a small preferred region.

4.b. The situation is opposite for the axino SWIMP scenario,whose signals can be found not only for the warm DM case butalso for the cold DM one.

jose a.r. cembranos et al- collider signatures of superwimp warm dark matter

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