Kaluza-Klein Dark Matter: a review
Géral!ne SERVANTService de Physique Théorique- CEA/Saclay
Based on work wi" -Tim Tait: hep-ph/0206071 (NPB)-Tim Tait: hep-ph/0206071 (NPB)hep-ph/0209262 (New J.Phys.)
-Bertone & Sigl: hep-ph/0211342 (PRD)
-Kaustubh Agashe: hep-ph/0403143 (PRL)hep-ph/0411254 (JCAP)
-Dan Hooper: to appear
ADD models
only gravity in bulk
R ~ meV-1 (flat)
Warped geometries
(Randall-Sundrum)
Hierarchy p
b solved
R ~ M-1
Pl M ~ TeVKK
but
(AdS)
- radion dark matter m~meV; (fine-tuned)
- branon dark matter (fine-tuned)
TeV X-dims-1
gauge bosons in bulk
all SM fields in bulk
R ~ TeV-1
(flat) "Universal" X-dims
- radion dark matter m~meV; (fine-tuned) - KK dark matter
WIMP!
- radion unstable
if GUT in bulk - KK dark matterWIMP!
WIMP KK dark ma#erSo far, two working models :
4 Universal Extra Dimensions (UED)WIMP = Lightest KK particle (LKP)
4 Warped GUTs
stability symmetry = KK parity
WIMP = Lightest charged particle (LZP) 3Z3Z symmetrystability symmetry =
+ a potential link between the LZP and baryogenesis...
Literature on KK dark matter: the complete list
Servant & Tait '02Cheng, Feng & Matchev '02Servant & Tait '02
Hooper & Kribs '02Bertone, Servant & Sigl '02Hooper & Kribs '04 Bergstrom, Bringmann, Eriksson & Gustafsson '04Baltz & Hooper '04Bergstrom, Bringmann, Eriksson & Gustafsson II '04
Agashe & Servant '04
Kakizaki, Matsumoto, Sato & Senami '05
Kolb & Slansky '84
Dienes, Dudas & Gherghetta '99
Thought about it, but in 1984 R ~TeV was inconceivable...
Detailed relic density calculationDirect and indirect detectionDirect detection
Prospects for neutrino telescopes
Positron excess
mentionned the idea in passingMohapatra& Perez-Lorenzana '02
Majumdar '02 Direct detection
Indirect detection
Indirect detection
A 2nd look at the relic density calculation
Agashe & Servant II '04
Hooper & Servant , upcoming
Model building, relic density, direct detection, collider signatures ...
Indirect detection
KK dark matter in
UED
Warped KK dark matter
-1
+ superWimp KK graviton papers
LKP dark matter Appelquist, Cheng & Dobrescu '01UED : ALL SM particles propagate into flat dimensions
in Universal Extra Dimensions
Conservation of momentum along extra dimension translates in 4D into conservation of KK number
by the orbifold we impose to recover a chiral theory
Other consequence of KK parity:Production of 1rst KK modes
only by pairs:
˛Weak bound on 1/R
LKP: most likely a 1B
Cheng, Matchev & Schmaltz'02
1-loop spectrum of 1rst KK modes
assuming:1/R=500 GeV, ΛR = 20, mh = 120 GeVand vanishing boundary terms at the cutoff Λ
Another intriguing possibility: LKP=KK graviton (see S. Su's talk)
γ 1(actually a )
)
Relic density pre!ctions
"natural KK resonance"hep-ph/0502059Kakizaki & al ,
4 Effect of 2nd KK modes
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
0 0.2 0.4 0.6 0.8 1 1.20
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
0 0.2 0.4 0.6 0.8 1 1.2
5d1 Flavor
3 Flavors
D = .05D = .01
Wh2 = 0.110 ± 0.006
mKK (TeV)
Wh2
4 Coannihilation effects
Servant-Tait
0
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
0 0.2 0.4 0.6 0.8 1 1.20
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
0 0.2 0.4 0.6 0.8 1 1.2
5d6d
Wh2 = 0.110 ± 0.006
mKK (TeV)
Wh2
4 Possible effect of additional dimension
Servant-Tait
Direct detectionExperimental limits :
LKP signal :
Cheng, Feng, Matchev '02
Servant, Tait '02
Particle physics model building in warped space
−2k |y|
Higgs oralternativedynamics for
breaking
TeVbrane
Planckbrane
4d graviton
Gauge fields and fermions in the bulk
y =
−
ds = dx + r dy
EW symmetry
2
Slice of AdS 5
y = 0 rp2 22
L RSU(2) SU(2) U(1)
5p
e
2005 favourite set-up:
Now embed this into a GUT + solve proton stability
4 High scale unification
4 hierarchy pb4 fermion masses
4 Dark matter
4 FRW cosmology
In GUTs ˛ MX,Ywhere ~ few TeV
˛ very fast proton decay
Solution: Break GUT by boundary conditions which split GUT multiplets zero modes=
SM fermions
Mass spectrum of KK fermions
Depends on:
4 type of boundary conditions on TeV and Planck branes
4 c-parameter (=5D bulk mass)(=localization of zero-mode wave function)
˛
For certain type of boundary conditions on fermions, there can be a hierarchy between the mass of KK
fermion and the mass of KK gauge bosons
Not a single KK scale
Ma$ %ectrum of light&t KK fermionvalue
10-1
1
10
10 2
10 3
-0.8 -0.7 -0.6 -0.5 -0.4 -0.3 -0.2 -0.110
-1
1
10
10 2
10 3
-0.8 -0.7 -0.6 -0.5 -0.4 -0.3 -0.2 -0.1
c < -1/2 :
mª0.83÷(c-1/2)÷(c+1/2)ekpr(c+1/2)MKK
-1/2 < c < -1/4 :
mª0.83÷(c+1/2)MKK
c > -1/4 :
mª0.65(c+1)MKK
c
m (G
eV)
MKK
10 TeV5 TeV 7 TeV
3 TeV
There exists a very light KK fermion as a consequence of the heaviness of the top quark
˛ LZP belongs to the multiplet containing SM top quarkand smallest c: c of the top quark
zero modes= SM fermions
10-4
10-3
10-2
10-1
1
10
10 2
10 10 2 10 310
-4
10-3
10-2
10-1
1
10
10 2
10 10 2 10 3
MKK=3 TeV
MKK=6 TeVWh2 = 0.110 ± 0.01
mLZP (GeV)
W h2 ¨ ƨ Æ annihilation is dominated by Z0 exchange annihilation is dominated byheavy KK gauge boson exchange
Relic density pre!ctions
Agashe-Servant '04
10-9
10-8
10-7
10-6
10-5
0.4 0.5 0.6 0.7 0.8 0.9 1 1.1 1.210
-9
10-8
10-7
10-6
10-5
0.4 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2
3 TeV
4 TeV
10 TeV
6 TeV
g10
sn-
LZP (
pb)
(spi
n-in
depe
nden
t)
CDMS limit (only applies for some range of wimp masses)
Wimp-nucleon elastic scattering cross section
(spin-independent)
masses of KK gauge bosons
Direct detection
Agashe-Servant '04
Co'ider Signatur&: exampl&4 W + 2 b+ E
T
6 W + 4 b+ ET
Indirect detection in neutrino telescopes
Hooper & Servant, in prep.
MKK=6 TeV
MKK=10 TeV
=4 TeVMKK
Large elastic scattering cross section: large capture rate in the SunEfficient production of neutrinos in annihilations
Cosmic positrons from LZP annihilations
Hooper & Servant, in prep.
Fit of the HEAT datafrom LZP annihilations
40 GeV LZP50 GeV LZP
A natural framework to relate Ωdark matter
Ωbaryons
andOur dark matter candidate carries baryon number! (B=1/3)
BUNIVERSE
= 0 = B + (-B)
carried by baryons
carried by anti-LZP
Assume an asymmetry between t and t is created via the out-of-equilibrium and CP-violating decay :
X' Xs tLZPanti-
Baryon number conservation leads to:
LZPn
LZPn -3 ( ) = n - n b b
Assuming efficient annihilation between and , and and :LZP LZP b b
b m
LZPnLZP
ρ= DM
≈ 6ρ
mLZP
≈ 18 GeV
-
LKP LSPLZP
n-ccn -3
B -( )Z3KK parity
(-1) n
R-parity
(-1) 3(B-L)+2S symmetry
gauge boson
Dirac fermion
Majorana fermion
nature
helicity suppressed(p-wave)
s-wave s-wave
20 GeV-few TeV~600-1000 GeV
4 LHC 4 Direct detection!
entire parameter
4 LHC!4 Indirect detection !
space is testable
4 Indirect 4 LHC fav()te detection
ma$ ran*annihilationcro$ section
detection
related to proton stability
~50 GeV-1 TeV
- Direct detection: CDMS, Edelweiss, Dama, Cresst, Zeplin, Xenon, Naiad ...
Abundance of experimental activity related to dark matter detection:
˛It is timely to study the distinctive signatures expected in different dark matter scenarios.
- Colliders
- Indirect detection:
Neutrino telescopes:
Gamma-ray telescopes:
Cosmic positron experiments:
LKPs, LZPs: viable alternatives to LSPs
To conclude
Hess, Veritas, Glast, Magic
Amanda, IceCube, AntaresHEAT, Pamela, AMS-2