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E T signatures and dark matter connection
Howard Baer
Florida State/ Oklahoma
⋆ Evidence for CDM⋆ Candidates for CDM
⋆ Neutralino CDM
• Relic density
• Direct and indirect detection of DM
⋆ NUSUGRA models
⋆ The gravitino problem
⋆ Gravitino CDM
⋆ Axino CDM
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Pillars of Big Bang cosmology: Hubble expansion
⋆ Theory: FRW universe
⋆ Hubble expansion
• HST key project
• type Ia supernovae probe
⋆ H 0dL = z + 12
(1− q0)z2 + · · ·⋆ H 0 = 72 km/sec/Mpc±10%
⋆ evidence for Λ > 0!
⋆ age of universe: ∼ 13.7 Gyrs
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Big Bang nucleosynthesis (BBN)
⋆ Thermal history
of universe:
⋆ Can compute light element
abundances: 4He, D, 3He, 7Li
• match to data:• ηB ≡ nB
nγ≃ 6× 10−10
• ηB from BBN
consistent with CMB results
? ? ? ?
? ? ? ?
@ @ @ @
@ @ @ @
3He/H p
4
He
2 3 4 5 6 7 8 9 101
0.01 0.02 0.030.005
C M
B
B B N
Baryon-to-photon ratio η × 10−10
Baryon density ΩBh2
D___H
0.24
0.23
0.25
0.26
0.27
10−4
10−3
10−5
10−9
10−10
2
5
7Li/H p
Yp
D/H p
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Cosmic microwave background (CMB)
⋆ COBE/WMAP/WMAP3, · · ·
⋆ anisotropies ∼ 10−5
⋆ can extract numerous
cosm. param’s from power spectrum
• flat (k = 0) universe: ρ = ρcas in inflation models
• contents of universe
∗ΩΛ
∼0.7
∗ Ωbaryons ∼ 0.04
∗ ΩCDM ∼ 0.25
∗ Ων ∼ tiny
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Baryogenesis: explaining ηB
⋆ SM electroweak baryogenesis: only if mH SM<∼ 50 GeV
⋆ MSSM: many more possibilities
•EW baryogenesis: need mt1 < mt; mh
<
∼120 GeV (Carena et al.)
• Affleck-Dine: decay of flat directions: baryo- or leptogenesis
• thermal leptogenesis: (Fukugita, Yanagida; Buchmueller, Plumacher, ...)
∗natural link to physics of massive neutrinos
∗ due to decay of heavy N states: N → Hℓ = N → H †ℓ∗ lepton asymmetry converted to baryon asymmetry via sphaleron effects
∗ get ηB ∼ 6× 10−10 if M N ∼ 1010 GeV
∗need reheat temp T R
∼1010 GeV
∗ overproduction of gravitinos if .1 <∼ mG<∼ 10 TeV
• leptogenesis via inflaton decay
⋆ can be constrained by ν /sparticle measurements
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Dark Matter in the universe
⋆ Binding of clusters
⋆ Galactic rotation curves
⋆ Gravitational lensing
⋆ Hot gas in clusters
⋆ CMB fluctuations
⋆ Large scale structure
⋆ flatness/BBN
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Best fit cosmology: concordance (ΛCDM ) model
•ΩBh2 = 0.022
±0.001
• Ωνh2 < 0.007 95% CL
• ΩΛh2 ∼ 0.38± 0.03
• ΩCDM h2 = 0.105± 0.01
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Candidates for Dark Matter
⋆ unseen baryons, e.g. BHs, brown dwarves, stellar remnants
– inconsistent with BBN element abundance calc’n
– limits from MACHO, EROS, OGLE
⋆ light neutrinos (= HDM )
⋆ axions/axinos
⋆ WIMPS
⋆ superWIMPS
⋆Q-balls
⋆ primordial BHs10
-3310
-3010
-2710
-2410
-2110
-1810
-1510
-1210
-910
-610
-310
010
310
610
910
1210
1510
18
mass (GeV)
10-39
10-36
10-33
10-30
10-27
10-24
10-21
10-18
10-15
10-12
10-9
10-6
10-3
100
103
106
109
1012
1015
1018
1021
1024
σ i n t
( p b )
Some Dark Matter Candidate Particles
neutrinosneutralinoKK photonbranonLTP
axion axino
gravitinoKK graviton
SuperWIMPs :
w i m p z
i l l aWIMPs :
B l a c k H o l e R e m
n a n t
Q-ball
fuzzy CDM
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Axions
⋆ PQ solution to strong CP problem in QCD⋆ pseudo-Goldstone boson from
PQ breaking at scale f a
⋆ non-thermally producedvia vacuum mis-alignment
• ma ∼ Λ2QCD/f a ∼ 10−6 − 10−1eV
• Ωah2 ∼ 1
2 6×10−6eV ma 7/6 h2
• astro bound: stellar cooling ⇒ ma < 10−1eV
• a couples to EM field: a− γ − γ coupling (Sikivie)
• axion microwave cavity searches
10-6
10-5
10-4
10-3
10-2
10-1
ma
( eV )
10-6
10-5
10-4
10-3
10-2
10-1
100
101
Ω a
h 2
measured : Ωh 2
= 0.105 + _ 0.01
axion relic density :
vacuum mis-alignment
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Axion microwave cavity searches
⋆ ongoing searches: ADMX experiment
• Livermore⇒ U Wash.
• Phase I: probe KSVZ
for ma ∼ 10−6 − 10−5 eV
• Phase II: probe DFSZfor ma ∼ 10−6 − 10−5 eV
• beyond Phase II:
probe higher values ma
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WIMPs: the WIMP miracle!
• Weakly Interacting Massive Particles• assume in thermal equil’n in early universe
• Boltzman eq’n:
– dn/dt = −3Hn− σvrel(n2 − n20)
• Ωh2 = s0ρc/h2
45πg∗
1/2xfM Pl
1σv
• ∼0.1 pbσv ∼ 0.1 mwimp100 GeV 2
• thermal relic ⇒ new physics at M weak!
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Some WIMP candidates
⋆ 4th gen. Dirac ν (excluded)
⋆ SUSY neutralino (χ or Z 1)
⋆ UED excited photon B1µ
⋆ little Higgs photon BH
⋆ little Higgs (theory space) N 1 (scalar)
⋆ warped GUTS: LZP KK fermion
⋆ branons
⋆ · · ·
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Neutralino dark matter
⋆ Why R-parity? natural in SO(10) SUSYGUTS if properly broken, or broken
via compactification (Mohapatra, Martin, Kawamura, · · ·)⋆ In thermal equilibrium in early universe
⋆ As universe expands and cools, freeze out
⋆ Number density obtained from Boltzmann eq’n
• dn/dt = −3Hn− σvrel(n2
− n2
0)• depends critically on thermally averaged annihilation cross section times
velocity
⋆ many thousands of annihilation/co-annihilation diagrams⋆ several computer codes available
• DarkSUSY, Micromegas, IsaReD (part of Isajet)
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Some neutralino (co)annihilation processes
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Relic density in minimal SUGRA model
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
Ωh2 0.094
0.094 Ωh2 0.1290.129 Ωh
2 0.5
G
G
G
NO REWSBLEP2
s t a u L
S P
m0
(GeV)
m 1 / 2
( G e
V )
mSUGRA,tanβ=10,A0=0,µ0,m
top=175GeV
δapos
x1010
:30,10,5,1 BF(b→sγ )x104:2,3
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
Ωh2 0.094
0.094 Ωh2 0.1290.129 Ωh
2 0.5
G
G
G
NO REWSBLEP2
s t a u L
S P
m0
(GeV)
m 1 / 2
( G e
V )
mSUGRA,tanβ=55,A0=0,µ0,m
top=175GeV
δapos
x1010
:30,10,5,1 BF(b→sγ )x104:2,3
HB, A. Belyaev, T. Krupovnickas and A. Mustafayev
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Main mSUGRA regions consistent with WMAP
⋆ bulk region (low m0, low m1/2)⋆ stau co-annihilation region (mτ 1 ≃ meZ1
)
⋆ HB/FP region (large m0 where |µ| → small )
⋆ A-funnel (2meZ1≃ mA, mH )
⋆ h corridor (2meZ1≃ mh)
⋆ stop co-annihilation region (particular A0 values mt1 ≃me
Z1)
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Constraints on SUSY models
⋆ LEP2:
– mh > 114.4 GeV for SM-like h
– mfW 1> 103.5 GeV
– meL,R > 99 GeV for mℓ −meZ1 > 10 GeV
⋆ BF (b → sγ ) = (3.55± 0.26)× 10−4 (BELLE, CLEO, ALEPH)
– SM theory: BF (b → sγ ) ≃ (3.0− 3.7)× 10−4
⋆ aµ = (g − 2)µ/2 (Muon g − 2 collaboration)– ∆aµ = (22± 10)× 10−10 (PDG value e+e−)
– ∆aSUSY µ ∝ m2
µµM i tanβ
M 4SUSY
⋆ BF (Bs → µ+µ−) < 1.5× 10−7 (CDF)
– constrains at very large tan β >∼ 50
⋆ ΩCDM h2 = 0.11± 0.01 (WMAP)
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Constraints as χ2 on mSUGRA model
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
0
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
mSUGRA, tgβ=10, µ0, A0=0, mtop=175 GeV
e+e
-input for δa
µ G LEP2 excluded
NO REWSB
s t a u
L S P
s q r t ( χ
2 )
m0 (TeV)
m 1 / 2
( G e
V )
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
0
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
mSUGRA, tgβ=55, µ0, A0=0, mtop=175 GeV
e+e
-input for δa
µ G LEP2 excluded
NO REWSB
s t a u
L S P
s q r t ( χ
2 )
m0 (TeV)
m 1 / 2
( G e
V )
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Direct detection of SUSY DM
⋆ Calculate neutralino-nucleus scattering
• calculate Z 1 − q or Z 1 − g scattering: take v → 0 limit
∗spin-dependent cross section couples to spin of nucleus: cancel
∗ spin-independent cross section ∝ A2: add∗ results usually quoted in terms of σSI ( Z 1 p) so results from different
target nuclei can be compared
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Current best limit: Xenon-10/CDMS results!
WIMP Mass [GeV/c2]
C
r o s s - s e c
t i o n
[ p b ] ( n
o r m a
l i s e d t o n u c
l e o
n )
080418114601
http://dmtools.brown.edu/
Gaitskell,Mandic,Filippini
101
102
103
10-10
10-9
10-8
10-7
10-6
10-5
080418114601
Baer et. al 2003XENON1T (proj)LUX 300 kg LXe Projection (Jul 2007)XENON100 (150 kg) projected sensitivitySuperCDMS (Projected) 25kg (7-ST@Snolab)WARP 140kg (proj)
SuperCDMS (Projected) 2-ST@SoudanCDMS Soudan 2007 projectedXENON10 2007 (Net 136 kg-d)CDMS: 2004+2005 (reanalysis) +2008 GeCDMS 2008 GeWARP 2.3L, 96.5 kg-days 55 keV thresholdDAMA 2000 58k kg-days NaI Ann. Mod. 3sigma w/DAMA 1996Edelweiss I final limit, 62 kg-days Ge 2000+2002+2003 limitDATA listed top to bottom on plot
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Indirect detection (ID) of SUSY DM: ν -telescopes
⋆ Z 1Z 1 → bb, etc. in core of sun (or earth): ⇒ ν µ → µ in ν telescopes
⋆ flux is largest when σ( Z 1 p) is largest– e.g. low mq or HB/FP region for mSUGRA
• experiments: Amanda, Icecube, Antares
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ID of SUSY DM: γ and anti-matter searches
• Z 1Z 1 → qq, etc. → γ in galactic core or halo
•Z 1Z 1
→qq, etc.
→e+ in galactic halo
• Z 1Z 1 → qq, etc. → ¯ p in galactic halo
• Z 1Z 1 → qq, etc. → D in galactic halo
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Rates for γ s, e+s, ¯ ps vs. m0 for fixed m1/2 = 550 GeV, tan β = 50
0 1000 2000 3000 4000
m0(GeV)
10−5
10−4
10−3
10−2
10−1
100
S / B ( e + )
0 5 10 15
r(kpc)
0
5
10
ρ ( G
e V c m −
3 )
default
NFW
Moore et al
Kravtsov et al
0 1000 2000 3000 4000
m0(GeV)
10−9
10−8
10−7
10−6
10−5
10−4
d
Φ p − / d E d Ω ( G
e V −
1 c
m −
2 s
− 1
s r −
1 )
0 1000 2000 3000 4000
m0(GeV)
10−12
10−10
10−8
10−6
10−4
Φ γ
( c
m −
2 s
− 1 )
a) b)
c) d)
• rates enhanced in A-funnel and HB/FP region (MHDM)
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Direct and indirect detection of neutralino DM
200
400
600
800
1000
1200
1400
1600
0 1000 2000 3000 4000 5000 6000 7000 8000
mSUGRA, A0=0 tanβ=10, µ0
m0(GeV)
m 1 / 2
( G e
V )
LEP
no REWSB
Z ~ 1 n o
t L S P
Φ(p-)=3x10
-7GeV
-1cm
-2s
-1sr
-1
(S/B)e+=0.01
Φ(γ )=10-10
cm-2
s-1
Φsun
(µ)=40 km-2
yr-1
G 0Ωh20.129
mh=114.4 GeVσ(Z
~
1p)=10-9
pb
L H C
LC1000
LC500
TEV
µ
D D
200
400
600
800
1000
1200
1400
1600
0 1000 2000 3000 4000 5000
mSUGRA, A0=0, tanβ=50, µ0
m0
(GeV)
m 1 / 2
( G e
V )
LEP
no REWSB
Z ~ 1 n o t L S P
Φ(p-) 3e-7 GeV
-1cm
-2s
-1sr
-1(S/B)
e+=0.01
Φ(γ )=10-10
cm-2
s-1
Φsun
(µ)=40 km-2
yr-1
G 0 Ωh2 0.129
mh=114.4 GeV
Φearth
(µ)=40 km-2
yr-1
σ(Z~
1p)=10-9
pb
L H C
LC1000
LC500
µ
D D
HB, Belyaev, Krupovnickas, O’Farrill
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SUGRA models with non-universal scalars
• Normal scalar mass hierarchy NMH: HB, Belyaev, Krupovnickas, Mustafayev
• m0(1) ≃ m0(2) ≪ m0(3) (preserve FCNC bounds)
•motivation: reconcile BF (b
→sγ ) with (g
−2)µ anomaly
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
200
400
600
800
1000
1200
1400
1600
1800
2000
0.5 1 1.5 2 2.5 3 3.5 4 4.5 5
0
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
mSUGRA, tgβ=30, µ0, A0=0, mtop=175 GeV,m01,2=100 GeV
e+e
-input for δaµ G LEP2 excluded
NO REWSB
s t a
u L S P
s q r t ( χ
2 )
m03 (TeV)
m 1 / 2
( G e
V )
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SUGRA models with non-universal Higgs mass (NUHM1)
• m2H u
= m2H d≡ m2
φ = m0: HB, Belyaev, Mustafayev, Profumo, Tata
• motivation: SO(10) SUSYGUTs where H u,d ∈ φ(10) while matter ∈ ψ(16)
• m2
φ ≫ m0 ⇒higgsino DM for any m0, m1/2
• m2φ < 0 ⇒ can have A-funnel for any tan β
10 -3
10 -2
10 -1
1
-3 -2 -1 0 1 2 m φ / m
0
Ω h 2
0
0.1
0.2 0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
-3 -2 -1 0 1 2 m φ / m
0
m ( T e V )
m0=300GeV, m
1/2=300GeV, tanβ=10, A
0=0, µ0, m
t=178GeV
WMAPm
A
mχ
µ
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NUHM2 (2-parameter case)
• m2H u = m2
H d = m0: HB, Belyaev, Mustafayev, Profumo, Tata
• motivation: SU (5) SUSYGUTs where H u ∈ φ(5), H d ∈ φ(5)
•can re-parametrize m2
H u, m2
H d
↔µ, mA (Ellis, Olive, Santoso)
• large S term in RGEs ⇒ light uR, cR squarks, meL < meR
NUHM2: m 0 =300GeV, m
1/2 =300GeV, tan β=10, A
0 =0, m
t =178GeV
100
200
300
400
500
600
700
800
900
0 250 500 750 1000 1250 1500 1750 2000
0
0.5
1
1.5
2
2.5
3
3.5
4
4.5
5
m A
(GeV)
µ ( G e V )
LEP2
s q r t ( χ 2 )
τ~
1
Ah
NUHM1
HS
mSUGRA
GS
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Gaugino mass non-universality
• M 1 = M 2 = M 3: HB, TK, AM, EP, SP, XT
• motivation: SUSYGUTs where gauge kinetic function transforms non-trivially
•M 2
∼M 1 at M GUT : mixed wino dark matter (MWDM)
• M 2 ≃ −M 1 at M GUT : bino-wino co-annihilation (BWCA)
-600 -400 -200 0 200 400 600
M1
(GeV)
10-5
10-4
10-3
10-2
10-1
100
101
102
103
104
Ω h
2
m0=300 GeV, m
1/2=300 GeV, tanβ=10, A
0=0, µ>0, m
t=178 GeV
-600 -400 -200 0 200 400 600
M1
(GeV)
0
0.2
0.4
0.6
0.8
1
R B ~
, W ~
w~
B
~
a) b)
WMAP
mSUGRA MWDMBWCA BWCA mSUGRA MWDM
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Gaugino mass non-universality: low M 3 case
• M 3 < M 1 ∼ M 2: HB, TK, AM, EP, SP, XT
• motivation: mixed-moduli AMSB models
• lower M 3 → low mq → low µ → mixed higgsino DM
-400 -200 0 200 400
M3
(GeV)
10-4
10-3
10-2
10-1
100
101
102
Ω h
2
m0=300 GeV, m
1/2=300 GeV, tanβ=10, A
0=0, µ>0, m
t=175 GeV
-400 -200 0 200 400
M3
(GeV)
0
0.2
0.4
0.6
0.8
1
R H ~
a) b)
WMAP
mSUGRA mSUGRAMHDM1 MHDM1
LEP2
Excluded
LEP2
Excluded
MHDM2 MHDM2
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Mixed higgsino DM from a high M 2 (HM2DM)
m 0
=300GeV, m 1/2
=300GeV, tan β=10, A0
=0, µ 0, m t =171.4GeV
10 -2
10 -1
1
-3 -2 -1 0 1 2 3
2007/07/07 11.40
WMAP
Ω h 2
0 0.10.2 0.3 0.4 0.5 0.6
0.7 0.8 0.9
1
-3 -2 -1 0 1 2 3
r 2
= M 2
/ m 1/2
R H
• high M 2 ⇒ low |µ| so get mixed higgsino DM but high mqL
• HB, Mustafayev, Summy, Tata
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Direct DM detection: well-tempered
Z 1 models
Spin-independent Direct Detection
10 -14
10 -13
10 -12
10 -11
10 -10
10 -9
10 -8
10 -7
10 -6
10 -5
200 400 600 800 1000 1200 1400
G
G
G
G
G
G
G
G
G
G
----⋅-⋅-⋅⋅⋅⋅⋅⋅
mSUGRA : µ > 0
mSUGRA : µ < 0
NUHM1µ
NUHM1A
MWDM1
MWDM2
BWCA2
LM3DM
HM2DM : M2 > 0
HM2DM : M2 < 0
Xenon-10
SuperCDMS 25 kg Xenon-100/LUX
Xenon-1 ton
m z1∼ (GeV)
σ S I
( p b )
• well-tempered
Z 1 models asymptote at σ(
Z 1 p) ∼ 10−8 pb!
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Compressed SUSY (Steve Martin)
• in models with low M 3 and A0 ∼ −M 1, the t1 becomes quite light
• Martin finds that if
– mt < meZ1
<
∼ mt + 100 GeV and
– meZ1+ 25 GeV
<∼ mt1<∼ meZ1
+ 100 GeV, then
• Z 1 Z 1
→tt is dominant dark matter annihilation mechanism in early Universe!
• implications for LHC, DD, IDD: (HB, Box, Park, Tata)
– light mg with t1 = NLSP
– collider signatures depend on whether t1→
c Z 1 or bW Z 1
– if t1 → c Z 1, then large E T + jets, but very low isolated lepton rates
– IDD halo annihilation signals enhanced since Z 1 Z 1 → tt → γ s, anti-matter
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Mixed modulus-AMSB models
⋆ KKLT model: type IIB superstring compactification with fluxes
• stabilize moduli/dilaton via fluxes and e.g. gaugino condensation on D7
brane
• introduce anti-D3 brane (uplifting potential; de Sitter universe with Λ > 0
• small SUSY breaking due to D3 brane
•mass hierarchy: mmoduli
≫m3/2
≫mSUSY
⋆ MSSM soft terms calculated by Choi, Falkowski, Nilles, Olechowski, Pokorski
⋆ phenomenology: Choi, Jeong, Okumura; Falkowski, Lebedev, Mambrini;
Kitano, Nomura
⋆ see also: HB, E. Park, X. Tata, T. Wang, JHEP0608, 041 (2006); PLB641,
447 (2006); JHEP0706, 033 (2007);
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α=6, m3/2
=12 TeV, tanβ=10, µ 0, mt=175 GeV
200
300
400
500
600
700
800
900
103
105
107
109
1011
1013
1015
1017
M1
M2
M3
a)
Q (GeV)
M a s s ( G e V
)
α=6, m3/2
=12 TeV, tanβ=10, µ 0, mt=175 GeV
-600
-400
-200
0
200
400
600
800
103
105
107
109
1011
1013
1015
1017
Hd
Hu
τR
τL
bR
tR
tL
eR
,e
L,
dR,
uR
uL b)
Q (GeV)
s i g n ( m i 2
) ⋅ √ | m i 2
| ( G e
V )
• GUT scale AMSB splitting of soft terms cancelled by RGE running:soft terms unify at “mirage” unification scale
• MM-AMSB contains BWCA, MWDM, LM3DM scenarios!
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SO(10) SUSYGUTs: motivation
⋆ In all the excitement of new models, it is easy to neglect the really good ideasfrom the past:
⋆ SUSYGUTs with SO(10) → SU (5) → SU (3)C × SU (2)L × U (1)Y :
• unification of forces• SO(10) naturally anomaly free
• explain ad-hoc SM hypercharge assignments (charge relations: e.g. why
m( proton) =−
me
• unification of matter in SO(10): matter ∈ ψ(16), higgs ∈ φ(10)
(simplest models)
•The 16-dim’l spinor rep of SO(10) contains all the matter in a single
generation of the SM, plus a right-handed neutrino state.
• break SO(10): get see-saw ν s!
• simplest models: t− b− τ Yukawa unification
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YU requires precision calculation of SUSY spectrum:
Hall, Rattazzi, Sarid; Pierce et al. (PBMZ)
• need full 2-loop RGE running
• RG-improved 1-loop effective potential evaluated at optimized scale
• t, b, τ threshold effects
• full set of 1-loop sparticle/Higgs mass corrections
• use Isajet/Isasugra 7.75 spectrum generator
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Running of Yukawa couplings: m16 = 10 TeV
1e+00 1e+02 1e+04 1e+06 1e+08 1e+10 1e+12 1e+14 1e+16
Q (GeV)
0.4
0.5
0.6
0.7
0.8
0.9
1
f i
f τ
f b
f t
• note shifts at Q = M SUSY !
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Y fi S !
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t − b− τ Yukawa unification in HS model!
• need m16 ∼ 5− 20 TeV
• need m10 ≃√
2m16
•A0
≃ −2m16
• tan β ≃ 50
• m1/2 ≪ m16
•inverted scalar mass hierarchy: Bagger et al.
• split Higgs needed for EWSB: m2H u
< m2H d
• Auto, HB, Balazs, Belyaev, Ferrandis, Tata
• HB, Kraml, Sekmen, Summy
• related work: Blazek, Dermisek, Raby (BDR); DRRR uses 1-loop SSB RGEs
and scalar pot’l minimization at Q = M Z
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S f R 1 i HS d l i h 0
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Scan for R ≃ 1 in HS model with µ > 0
• R = max(f t, f b, f τ )/min(f tf b, f τ )
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Special SUSY spectrum from Yukawa unified models
• first/second gen. squarks/sleptons ∼ 5− 20 TeV
• third gen. scalars, µ, mA ∼ 1− 2 TeV
• gluinos ∼ 350− 500 GeV
• charginos ∼ 100− 160 GeV
• Z 1 or χ1
∼50−
80 GeV
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Problem: Ω eZ 1h2 ∼ 103 − 105× WMAP
•for R
≃1, then ΩeZ1h2
>
∼102!
• higher than measured value by 103 − 105
• Does this rule out Yukawa-unified SUSY?
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Solution: axino a dark matter
• invoke axion solution to strong CP problem
•axino is spin 1
2
element of saxion/axion/axino supermultiplet
• 10−6 eV < ma < 10−2 eV
• 100 keV < ma <∼ 10 GeV
• for our case, Z 1 → aγ with τ eZ1 ∼ 0.03 sec
• can shed large factors of relic density:
•Ωah2
∼mam eZ1
ΩeZ1h2:
⇒warm DM for ma < 1
−10 GeV (JLM)
• also generate thermal component for axino DM depending on T R: ⇒ CDM
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Consistent cosmology for SUSY SO(10): gravitino problem
• gravitino problem in generic SUGRA models: overproduction of G followed by
late G decay can destroy successful BBN predictons: upper bound on T R
(see Kohri, Moroi, Yotsuyanagi; Cybert, Ellis, Fields, Olive)
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Leptogenesis via inflaton decay
• Upper bound on T R from BBN is below that for successful thermal
leptogenesis: need T R>
∼ 1010
GeV (Buchmuller, Plumacher)
• Alternatively, one may have non-thermal leptogenesis where inflaton
φ → N iN i decay (Lazarides,Shafi; Kumekawa, Moroi, Yanagida)
• additional source of N i in early universe allows lower T R:
nBs≃ 8.2× 10−11 ×
T R
106 GeV
2mN 1
mφ
mν30.05 eV
δeff (1)
• WMAP observation: nb/s ∼ 0.9× 10−10 ⇒ T R>
∼ 106 GeV
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Cold and warm axino DM in the universe
• Non-thermal axino production via
Z 1 → aγ decay:
⇒ warm DM for ma<
∼ 1 GeV (Jedamzik, Lemoine, Moultaka)
• thermal production of a: cold DM for ma > .1 MeV
(Brandenberg, Steffen)
ΩTP a h2 ≃ 5.5g6s ln1.108
gs
1011 GeVf a/N
2 ma0.1 GeV
T R104 GeV
(2)
• with 0.1 ≃ Ωah2 = ΩTP a h2 + mam eZ1
ΩeZh2, can calculate value of T R needed
given a PQ breaking scale f a/N ∼ 1011 GeV
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Consistent cosmology for SO(10) SUSY GUTs with a DM
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Consistent cosmology for SO(10) SUSY GUTs with a DM
• Happily, T R falls into the right range to give cold axino DM with a smalladmixture of warm axino DM, preserve BBN predictions (solving the gravitino
problem) and have non-thermal leptogenesis!
•See HB and H. Summy, arXiv:0803.0510 (2008)
1e-05 0.0001 0.001 0.01
ma~
(GeV)
1e+06
1e+07
1e+08
1e+09
T R
( G e
V ) BBN/gravitino
NT leptogenesis
warm a~DM
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SuperWIMPs (e g G in SUGRA or G in UED)
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SuperWIMPs (e.g. G in SUGRA or G in UED)
⋆ mG = F/√3M ∗ ∼ TeV in Supergravity models
• usually G decouples (but see Moroi et al. for BBN constraints)
• if G is LSP, then calculate NLSP abundance as a thermal relic: ΩNLSP h2
• Z 1 → hG, Z G, γ G or τ 1 → τ G possible
∗ lifetime τ NLSP ∼ 104 − 108 sec
∗ constraints from BBN, CMB not too severe
∗DM relic density is then Ω ˜
G=
mG
mNLSP ΩNLSP
+ ΩTP G
(T R
)
∗ Feng, Rajaraman, Su, Takayama; Ellis et al; Buchmuller et al.
• G undetectable via direct/indirect DM searches
•unique collider signatures:
∗ τ 1=NLSP: stable charged tracks
∗ can collect NLSPs in e.g. water (slepton trapping)
∗ monitor for NLSP → G decays
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SUGRA d l b d MSSM NMSSM
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SUGRA models beyond MSSM: NMSSM
⋆ Add extra singlet SF S
• motivation: introduce µ parameter via SUSY breaking
•3 neutral scalar higgs, 2 pseudoscalars and 5 neutralinos
0 200 400 600 800
µ [GeV]
0
200
400
600
800
M 2
[ G e V
]
W M
A P
Ωh2= 1
Ωh2= 0.02
Belanger, Boudjema, Hugonie, Pukhov, Semenov
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Conclusions
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Conclusions
⋆ Overwhelming evidence for CDM in the universe
⋆ Numerous candidate CDM particles
• Axions: searches ongoing (ADMX group)
⋆ SUSY LSP: thermal relic from Big Bang
⋆ Various regions ⇒ distinct collider/DM signatures
⋆ Direct/ indirect DM detection prospects
⋆ Detection at colliders: Tevatron, LHC, ILC
⋆ Beyond mSUGRA:
•NMH, NUHM1, NUHM2, MWDM, BWCA, low M 3, high M 2, comp.
SUSY, SO(10)
• axino a or gravitino G as dark matter
• NMSSM
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