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Universums g

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Can even be used to discriminate between the LKP and a Majorana dark matter candidate! ... To explain the HEAT data, a BF of several 100 would be needed (for mB ... – PowerPoint PPT presentation

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Title: Universums g


1
Kaluza-Klein (KK) Dark Matter
Torsten Bringmann, SISSA
ENTApP Visitor Program and Workshop on Dark
Matter, SISSA, Trieste, 12-21 Oct 05
2
Outline
a viable dark matter candidate
- the positron peak
- the gamma-ray spectrum
- antiprotons
3
Outline
Why should we be interested in this particular
dark matter candidate?
4
Extra dimensions the basic idea
Compactify extra dimensions on some small scale
R
2 R
Fig. Greene 00
5
Universal Extra dimensions (UED)
Appelquist, Cheng Dobrescu, PRD 01
6
The field content in 4D
At the first KK level, one finds the following
mass eigenstates
Vector bosons
Scalars
Ghosts
Fermions
7
The lightest Kaluza-Klein particle
Does this give a viable dark matter candidate?
8
What is the LKP?
Cheng, Matchev Schmaltz, PRD 02
At tree level, the mass of the KK modes is given
by
The LKP is given by the B(1)
9
The LKP as a dark matter particle
The WMAP bound translates into
10
Collider bounds
- Direct non-detection
R-1 ? 300 GeV
Appelquist, Cheng Dobrescu, PRD 01
Agashe, Deshpande Wu, PL B 01
- Electroweak precision tests
11
Indirect detection
B(1) B(1) annihilation ratios at tree level
- 59 into leptons
Compare to SUSY!
- 35 into quarks
- 4 into neutrinos
- 2 into gauge and Higgs bosons
12
The positron peak
Appearance of a smoking gun signature in the
spectrum.
HK
13
The gamma-ray spectrum
Bergström, T.B., Eriksson Gustafsson, PRD 05
At high energies, the gamma-ray spectrum is
dominated by internal bremsstrahlung from final
state leptons
This gives a nice signature to look for.
14
The H.E.S.S. data
Expected gamma-ray flux from the galactic center
15
Can one see the photon peak?
Bergström, T.B., Eriksson Gustafsson, JCAP 05
As for SUSY, direct annihilation into ?? or Z? is
loop-suppressed.
16
Antiprotons from KK dark matter
Expected fluxes are in general too low to be seen

17
Antiprotons from KK dark matter
Expected fluxes are in general too low to be seen

Allowing for clumpy halo distributions, however,
PAMELA and AMS will be able to see a
characteristic distortion in the spectrum.
mB(1) 800 GeV, boost-factor 100
T.B. 05
18
Neutrinos
In contrast to SUSY, neutrinos are directly
produced in LKP annihilations (branching ratio
4).
19
Direct detection
Single nucleon cross sections spin-independent/s
pin-dependent mp/mB(1)
Detection rates spin-independent/spin-dependent

20
Upcoming direct-detection experiments
Servant Tait, NJP 02
Ge detectors
Xe detectors
21
Conclusions
The LKP appears as a natural dark matter
candidate in the UED model
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