supersymmetric dark matter: direct, indirect and …baer/okstate.pdf⋆ part 2: models/implications...
TRANSCRIPT
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Supersymmetric Dark Matter:
Direct, Indirect and Collider Searches
Howard Baer
University of Oklahoma
OUTLINE
⋆ The Standard Model
⋆ Inconsistencies
⋆ Supersymmetry
⋆ Dark matter (DM)
• neutralino, axion/axino, gravitino
⋆ The Hunt for DM at LHC
⋆ direct DM searches
⋆ indirect DM searches
Howie Baer, Oklahoma State University colloquium, April 16, 2009 1
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The Standard Model of Particle Physics
⋆ gauge symmetry: SU(3)C × SU(2)L × U(1)Y ⇒ g, W±, Z0, γ
⋆ matter content: 3 generations quarks and leptons
u
d
L
uR, dR;
ν
e
L
, eR (1)
⋆ Higgs sector ⇒ spontaneous electroweak symmetry breaking:
φ =
φ+
φ0
(2)
⋆ ⇒ massive W±, Z0, quarks and leptons
⋆ L = Lgauge + Lmatter + LY uk. + LHiggs: 19 parameters
⋆ good-to-excellent description of (almost) all accelerator data!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 2
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Shortcomings of SM
Data
⋆ neutrino masses and mixing
⋆ baryogenesis (matter anti-matter asymmetry)
⋆ cold dark matter
⋆ dark energy
Theory
⋆ quadratic divergences in scalar sector ⇒ fine-tuning
⋆ origin of generations
⋆ explanation of masses/ mixing angles
⋆ origin of gauge symmetry/ quantum numbers
⋆ unification with gravity
Howie Baer, Oklahoma State University colloquium, April 16, 2009 3
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The supersymmetry alternative
Supersymmetry: bosons⇔ fermions
⋆ SUSY is a space-time symmetry!
⋆ space-time xµ ⇒ (xµ, θi) i = 1, · · · , 4 superspace
⋆ fields ψ ⇒ φ ∋ (φ, ψ) superfields
⋆ gauge fields Aµ ⇒ W ∋ (λ, Aµ) gauge superfields
⋆ superfield formalism ⇒ general form for Lagrangian of (globally)
supersymmetric gauge theory: quadratic divergences cancel!
⋆ SUSY can be broken by soft SUSY breaking terms: maintain cancellation of
quadratic divergences
Howie Baer, Oklahoma State University colloquium, April 16, 2009 4
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Weak Scale Supersymmetry
HB and X. Tata
Spring, 2006; Cambridge University Press
⋆ Part 1: superfields/Lagrangians
– 4-component spinor notation for exp’ts
– master Lagrangian for SUSY gauge theories
⋆ Part 2: models/implications
– MSSM, SUGRA, GMSB, AMSB, · · ·– dark matter density/detection
⋆ Part 3: SUSY at colliders
– production/decay/event generation
– collider signatures
– R-parity violation
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Minimal Supersymmetric Standard Model (MSSM)
⋆ Adopt gauge symmetry of Standard Model
• spin 1
2gaugino for each SM gauge boson
⋆ SM fermions ∈ chiral scalar superfields: ⇒ scalar partner for each SM
fermion helicity state
• electron ⇔ eL and eR
⋆ two Higgs doublets to cancel triangle anomalies
⋆ add all admissible soft SUSY breaking terms
⋆ resultant Lagrangian has 124 parameters!
⋆ Lagrangian yields mass eigenstates, mixings, Feynman rules for scattering and
decay processes
⋆ predictive model!
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Supergravity (SUGRA)
⋆ eiαQ with α(x): local SUSY transformation
• forces introduction of spin 2 graviton and spin 3
2gravitino
• resultant theory ⇒ General Relativity in classical limit!
⋆ rules for Lagrangian in supergravity gauge theory: Cremmer et al. (1983)
⋆ fertile ground: supergravity ∪ grand unification: LE limit of superstring?
⋆ minimal supergravity model (mSUGRA)
⋆ m0, m1/2, A0, tan β, sign(µ)
• m0 = mass of all scalars at Q = MGUT
• m1/2 = mass of all gauginos at Q = MGUT
• A0 = trilinear soft breaking parameter at Q = MGUT
• tanβ = ratio of Higgs vevs
• µ = SUSY Higgs mass term; magnitude determined by REWSB!
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Some successes of SUSY GUT theories
⋆ SUSY divergence cancellation maintains hierarchy between GUT scale
Q = 1016 GeV and weak scale Q = 100 GeV
⋆ gauge coupling unification!
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Gauge coupling evolution
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Some successes of SUSY GUT theories
⋆ SUSY divergence cancellation maintains hierarchy between GUT scale
Q = 1016 GeV and weak scale Q = 100 GeV
⋆ gauge coupling unification!
⋆ Lightest Higgs mass mh<∼ 135 GeV as indicated by radiative corrections!
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Precision electroweak data and the Higgs mass:
160 165 170 175 180 185mt [GeV]
80.20
80.30
80.40
80.50
80.60
80.70
MW
[GeV
]
SM
MSSM
MH = 114 GeV
MH = 400 GeV
light SUSY
heavy SUSY
SMMSSM
both models
Heinemeyer, Hollik, Stockinger, Weber, Weiglein ’08
experimental errors 68% CL:
LEP2/Tevatron (today)
Tevatron/LHC
S. Heinemeyer et al.
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Some successes of SUSY GUT theories
⋆ SUSY divergence cancellation maintains hierarchy between GUT scale
Q = 1016 GeV and weak scale Q = 100 GeV
⋆ gauge coupling unification!
⋆ Lightest Higgs mass mh<∼ 130 GeV as indicated by radiative corrections!
⋆ radiative breaking of EW symmetry if mt ∼ 100 − 200 GeV!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 12
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Soft term evolution and radiative EWSB
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Some successes of SUSY GUT theories
⋆ SUSY divergence cancellation maintains hierarchy between GUT scale
Q = 1016 GeV and weak scale Q = 100 GeV
⋆ gauge coupling unification!
⋆ Lightest Higgs mass mh<∼ 130 GeV as indicated by radiative corrections!
⋆ radiative breaking of EW symmetry if mt ∼ 100 − 200 GeV!
⋆ dark matter candidate: lightest neutralino Z1
⋆ stablize neutrino see-saw scale vs. weak scale
⋆ SO(10) SUSY GUT: baryogenesis via leptogenesis
⋆ can give dark energy via CC Λ (but need huge fine-tuning...)
• SUGRA = low energy limit of superstring?
• stringy multiverse: anthropic selection of small CC?
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Evidence for dark matter in the universe
⋆ binding of galactic clusters (Zwicky, 1930s)
⋆ galactic rotation curves
⋆ large scale structure formation
⋆ inflation ⇒ Ω = ρ/ρc = 1
⋆ gravitational lensing
⋆ anisotropies in cosmic MB (WMAP)
⋆ surveys of distant galaxies via SN (DE)
⋆ Big Bang nucleosynthesis
• ΩΛ ≃ 0.7
• ΩCDM ≃ 0.25
• Ωbaryons ≃ 0.045 (dark baryons ∼ 0.040)
• Ων ≃ 0.005
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Dark matter versus dark energy
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SUSY dark matter
⋆ R-parity conservation⇒ conserved B and L ⇒ proton stability
• R(particle) = 1; R(sparticle) = −1
⋆ Naturally occurs in SO(10) SUSY GUT theories
⋆ Some consequences:
• Sparticles are produced in pairs
• Sparticles decay to other sparticles
• Lightest SUSY particle (LSP) is absolutely stable (good candidate for dark
matter)
⋆ LSP must be charge, color neutral (bound on cosmological relics)
⋆ Sneutrino would have been detected in direct detection experiments
⋆ lightest neutralino Z1 is LSP in wide range of models
⋆ Z1 is weakly interacting, massive particle (WIMP)
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Calculating the relic density of neutralinos
⋆ At very high T , neutralinos in thermal equilibrium with cosmic soup
⋆ As universe expands and cools, expansion rate exceeds interaction rate
(freeze-out)
⋆ number density is governed by Boltzmann eq. for FRW universe
• dn/dt = −3Hn− 〈σvrel〉(n2 − n20)
• Ω eZ1h2 = s0
ρc/h2
(45
πg∗
)1/2xf
mP l
1
〈σv〉
• ΩCDMh2 ∼ 0.1 ⇒ 〈σv〉 ∼ 0.9 pb!
• 〈σv〉 = πα2/8m2 ⇒ m ∼ 100 GeV
• “The WIMP miracle!”: cosmic motivation for new physics at weak scale
⋆ SUSY: 1722 annihilation/co-annihilation reactions; 7618 Feynman diagrams
⋆ IsaReD program (HB, A. Belyaev , C. Balazs)
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Results of χ2 fit using τ data for aµ:
mSugra with tanβ = 10, A0 = 0, µ > 0
0
250
500
750
1000
1250
1500
1750
2000
0 1000 2000 3000 4000 5000 6000
mSugra with tanβ = 10, A0 = 0, µ > 0
0
250
500
750
1000
1250
1500
1750
2000
0 1000 2000 3000 4000 5000 6000
-2
0
2
4
6
8
m0 (GeV)
m1/
2 (G
eV)
ln(χ
/DO
F)
No REWSB
Ζ~
1 no
t LSP
mh=114.1GeV LEP2 excluded
SuperCDMS CDMSII CDMS
mSugra with tanβ = 54, A0 = 0, µ > 0
0
250
500
750
1000
1250
1500
1750
2000
0 1000 2000 3000 4000 5000 6000
mSugra with tanβ = 54, A0 = 0, µ > 0
0
250
500
750
1000
1250
1500
1750
2000
0 1000 2000 3000 4000 5000 6000
0
2
4
6
8
10
12
14
m0 (GeV)m
1/2
(GeV
)
ln(χ
2 /DO
F)
No REWSB
Ζ~
1 no
t LSP
mh=114.1GeV LEP2 excluded
SuperCDMS CDMSII CDMS
HB, C. Balazs: JCAP 0305, 006 (2003)
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Axions
⋆ PQ solution to strong CP problem in QCD
⋆ pseudo-Goldstone boson from
PQ breaking at scale fa ∼ 109 − 1012 GeV
⋆ non-thermally produced
via vacuum mis-alignment as cold DM
• ma ∼ Λ2QCD/fa ∼ 10−6 − 10−1eV
• Ωah2 ∼ 1
2
[6×10
−6eVma
]7/6
h2
• astro bound: stellar cooling ⇒ ma < 10−1eV
• a couples to EM field: a− γ − γ coupling (Sikivie)
• axion microwave cavity searches
10-5
10-4
10-3
ma (eV)
10-5
10-4
10-3
10-2
10-1
100
Ωah2 (
vacu
um m
is-a
lignm
ent)
109
1010
1011
1012
fa
/N (GeV)
WMAP 5: ΩCDM
h2 = 0.110 ± 0.006
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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 DFSZ
for ma ∼ 10−6 − 10−5 eV
• beyond Phase II:
probe higher values ma
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Axions + SUSY ⇒ Axino a dark matter
• axino is spin-1
2element of axion supermultiplet (R-odd; can be LSP)
• ma model dependent: keV→ GeV
• Z1 → aγ
• non-thermal a production via Z1 decay:
• axinos inherit neutralino number density
• ΩNTPa h2 = ma
m eZ1
Ω eZ1
h2:50 60 70 80 90
mχ~1
0 (GeV)
10-5
10-4
10-3
10-2
10-1
100
101
τ (s
)
fa /N = 10
9 GeV
fa /N = 1010
GeV
fa /N = 10
11 GeV
fa /N = 10
12 GeV
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Thermally produced axinos
⋆ If TR < fa, then axinos never in thermal equilibrium in early universe
⋆ Can still produce a thermally via radiation off particles in thermal equilibrium
⋆ Brandenberg-Steffen calculation:
ΩTPa h2 ≃ 5.5g6
s ln
(1.108
gs
)(1011 GeV
fa/N
)2 ( ma
0.1 GeV
) (TR
104 GeV
)(3)
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
ma~ (GeV)
104
105
106
107
108
109
1010
TR (
GeV
)
fa /N = 10 12
GeVfa /N = 10 11
GeVfa /N = 10 10
GeV
hot warm cold
NT leptogenesis
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Gravitinos: spin-3
2partner of graviton
• gravitino problem in generic SUGRA models: overproduction of G followed by
late G decay can destroy successful BBN predictons: upper bound on TR
(see Kawasaki, Kohri, Moroi, Yotsuyanagi; Cybert, Ellis, Fields, Olive)
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Gravitinos as dark matter: again the gravitino problem
• neutralino production in generic SUGRA models: followed by late time
Z1 → G+Xdecays can destroy successful BBN predictons:
(see Kawasaki, Kohri, Moroi, Yotsuyanagi)
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Gravitino dark matter: if one can avoid gravitino problem
⋆ mG = F/√
3M∗ ∼ TeV in Supergravity models
• if G is LSP, then calculate NLSP abundance as a thermal relic: ΩNLSPh2
• Z1 → hG, ZG, γG or τ1 → τG possible
∗ lifetime τNLSP ∼ 104 − 108 sec
∗ also produce G thermally (depends on re-heat temp. TR)
∗ DM relic density is then ΩG =mG
mNLSPΩNLSP + ΩTP
G
∗ Feng et al.; Ellis et al.; Brandenberg+Steffen; Buchmuller et al.
• G undetectable via direct/indirect DM searches
• unique collider signatures are possible:
∗ τ1=NLSP: stable charged tracks
∗ can collect NLSPs in e.g. water (slepton trapping)
∗ monitor for NLSP → G decays
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Production of sparticles at CERN LHC
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Sparticle cascade decays
400
600
800
1000
1200
1400
1600
1800
2000
10-2
10-1
1 10 102
Br (%)
Mas
s s
cale
(G
eV)
g~ (2060)
q ~
L (≈1857)
q ~
R (≈1770)
b ~
2 (1690) t
~
2 (1689) b
~
1 (1619)
t ~
1 (1449)
W ~ ±
2 (1067) Z
~ 4 (1066)
Z ~
3 (1056)
W ~ ±
1 (754) Z
~ 2 (754)
τ ~
2 (726) ν
~
τ (712)
τ ~
1 (442) Z
~ 1 (395)
Z ~
1 qq (27.0 %)
Z ~
1 τνWbb (12.1 %)
Z ~
1 ττWWbb (8.4 %)
Z ~
1 WWbb (7.4 %)
Z ~
1 τνqq (5.9 %)
Z ~
1 τνWWWbb (4.1 %)
Z ~
1 ττbb (2.9 %)
Z ~
1 ττqq (2.9 %)
Z ~
1 τνZWbb (2.8 %)
Z ~
1 τνhWbb (2.6 %)
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Event generation for sparticles
~
~
~Z1
~Z1
g
Hadrons
Remnants
q
p
p
1
23
4
5
Event generation in LL - QCD
1) Hard scattering / convolution with PDFs
2) Intial / final state showers
3) Cascade decays
4) Hadronization
5) Beam remnants
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Isajet v7.79 for sparticle event generation
⋆ Isajet (1979), by F. Paige and S. Protopopescu
⋆ Isajet 7.0 (1993) -7.75: FP, SP, HB and X. Tata
• Isasugra subprogram: SUGRA models (and others)⇒ sparticle masses,
mixings, decay rates
⋆ SUSY and SM event generation for hadron colliders
⋆ e+e− colliders
• polarized beams
• bremsstrahlung/ beamstrahlung
⋆ IsaTools: Ω eZ1h2, (g − 2)µ, BF (b→ sγ), BF (Bs → µ+µ−), σ(Z1p)
⋆ Les Houches event output: 7.78
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Simulated sparticle production event at LHC
S. Abdullin Oct.2000
GEANT figure
mSUGRA : m 0 = 1000 GeV, m 1/2 = 500 GeV, A 0= 0, tan β = 35, µ > 0
m g ~ = 1266 GeV
m u ~ = 1450 GeV
m t ~ = 1026 GeV
m
~ = 410 GeV 1
L
Z 2
m ~ = 214 GeVZ
1
m h = 119 GeV
g ~
t ~
1 t -
W -
+ b -
T = 113 GeV)
s + c -
~W +
2 + b ~W +
1 + Z ν ν-
( jet4, E
T = 79 GeV) ( jet5, E
T = 536 GeV)( jet3, E
~Z
1 W +
+ τ e ν
+ +
u ~
L ~Z
2 + u T = 1196 GeV)( jet6, E
~Z
1 + h
b -
T = 320 GeV)( jet2, ET = 206 GeV)( jet1, E b
ν
S.
Abd
ullin
, A
. Nik
iten
ko
b-jet 1
b-jet 2 Z 1
Z 1
b-jet 3
b-jet 4
jet 5
jet 6
E T
miss= 380 GeV
~
~
5
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e+e− → W+
1 W−
1 → (qq′Z1) + (eνeZ1) at linear collider
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Sparticle reach of all colliders with relic density
200
400
600
800
1000
1200
1400
1600
0 1000 2000 3000 4000 5000 6000 7000 8000
mSugra with tanβ = 10, A0 = 0, µ > 0
m0 (GeV)
m1/
2 (G
eV)
LHC
Tevatron
LC 500
LC 1000
Ωh2< 0.129
LEP2 excluded
200
400
600
800
1000
1200
1400
1600
0 1000 2000 3000 4000 5000 6000 7000
mSugra with tanβ = 45, A0 = 0, µ < 0
m0 (GeV)m
1/2
(GeV
)
LHC
Tevatron
LC 500
LC 1000
Ωh2< 0.129
LEP2 excluded
HB, Belyaev, Krupovnickas, Tata: JHEP 0402, 007 (2004)
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Early SUSY discovery at LHC with just 0.1 fb−1?
• To make 6ET cut, complete knowledge of detector needed
– dead regions
– “hot” cells
– cosmic rays
– calorimeter mis-measurement
– beam-gas events
• Can we make early discovery of SUSY at LHC without 6ET ?
• Expect SUSY events to be rich in jets, b-jets, isolated ℓs, τ -jets,....
• These are detectable, rather than inferred objects
• Answer: YES! See HB, Prosper, Summy, arXiv:0801.3799
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D0 saga with missing ET
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Simple cuts: ≥ 4 jets plus isolated leptons
• 6ET not really necessary
0 5# of Isolated Leptons
0.1
1
10
100
1000
10000
1e+05
1e+06
1e+07
σ (f
b)
SO10ptA(9202.87,62.498,-19964.500,49.1,171)QCD JetsttW+jetsZ+jetsWW, WZ, ZZSum of Backgrounds
No. of Isolated LeptonsCuts C1a
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Cuts C1′ plus ≥ 2 OS/SF ℓ
0 50 100 150m
ll (GeV)
0
10
20
30
40
dσ/d
mll (
fb/G
eV)
SO10ptA + BGQCD JetsttW+jetsZ+jetsWW, WZ, ZZSum of Backgrounds
Cuts C1a
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Precision measurements at LHC: Atlas and CMS
• Meff = 6ET + ET (j1) + · · · + ET (j4) sets overall mg, mq scale
• m(ℓℓ) < meZ2−meZ1
mass edge
• m(ℓℓ) distribution shape
• combine m(ℓℓ) with jets to gain m(ℓℓj) mass edge: info on mq
• further mass edges possible e.g. m(ℓℓjj)
• Higgs mass bump h→ bb likely visible in 6ET + jets events
• in favorable cases, may overconstrain system for a given model
⋆ methodology very p-space dependent
⋆ some regions are very difficult e.g. HB/FP
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International linear e+e− collider (ILC)
⋆ A linear e+e− collider with√s = 0.5 − 1 TeV is highest priority project for
HEP beyond LHC! Why?
• All beam energy ⇒ collision (aside from brem/beamstrahlung losses)
• beam energy known
• clean collision environment
• low (electroweak) background levels
• adjustable beam energy (threshold scans)
• e− and possibly e+ beam polarization
⋆ ILC will be ideal machine to perform precision spectroscopy of any new (EW
interacting) matter states (provided they are kinematically accessible)!
⋆ timeline: decision-2012; ready-2025?
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Precision sparticle measurements at a e+e− linear collider
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Direct detection of SUSY DM
⋆ Direct search via neutralino-nucleon scattering
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Direct detection of neutralino DM: the race is on!
WIMP Mass [GeV/c2]
Cro
ss-s
ectio
n [p
b] (
norm
alis
ed to
nuc
leon
)
080418114601
http://dmtools.brown.edu/ Gaitskell,Mandic,Filippini
101
102
103
10-10
10-9
10-8
10-7
10-6
10-5
080418114601Baer 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
⋆ Z1Z1 → bb, etc. in core of sun (or earth): ⇒ νµ → µ in ν telescopes
• Amanda, Icecube, Antares
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ID of SUSY DM: γ and anti-matter searches
• Z1Z1 → qq, etc.→ γ in galactic core or halo
• Z1Z1 → qq, etc.→ e+ in galactic halo
• Z1Z1 → qq, etc.→ p in galactic halo
• Z1Z1 → qq, etc.→ D in galactic halo
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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, µ>0
m0(GeV)
m1/
2(G
eV)
LEP
no REWSB
Z~
1 no
t LS
P
Φ(p-)=3x10-7 GeV-1 cm-2 s-1 sr-1
(S/B)e+=0.01
Φ(γ)=10-10 cm-2 s-1
Φsun(µ)=40 km-2 yr-1
0<Ωh2<0.129
mh=114.4 GeV
σ(Z~
1p)=10-9 pb
LHC
LC1000
LC500
TEV
µD
D
200
400
600
800
1000
1200
1400
1600
0 1000 2000 3000 4000 5000
mSUGRA, A0=0, tanβ=50, µ<0
m0 (GeV)m
1/2
(GeV
)
LEP
no REWSB
Z~
1 no
t LS
P
Φ(p-) 3e-7 GeV-1 cm-2 s-1 sr-1 (S/B)e+=0.01
Φ(γ)=10-10 cm-2 s-1 Φsun(µ)=40 km-2 yr-1
0< Ωh2< 0.129
mh=114.4 GeV
Φearth(µ)=40 km-2 yr-1 σ(Z~
1p)=10-9 pb
LHC
LC1000
LC500
µ
DD
HB, Belyaev, Krupovnickas, O’Farrill: JCAP 0408, 005 (2004)
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Impact of DM direct/indirect detection on LHC program
• Extend reach in σSI ∼ 10−9 − 10−10 pb
– explore thoroughly region of MHDM, possibly MWDM
• after discovery, extract mwimp?
– meZ1sets absolute mass scale for SUSY particles-
– combine with LHC mass edges to gain LHC absolute sparticle masses
– learn if Z1 is absolutely stable: R-conservation
• IceCube turn-on can discover/verify especially MHDM
• knowledge of LHC spectra, σSI , σSD combined with possible gamma ray
signals may allow map of dark matter distribution in the galaxy
• role of p, e+, D signals
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Models beyond mSUGRA
⋆ Normal scalar mass hierarchy
– split scalar generations m0(1) ≃ m0(2) ≪ m0(3)
– resolves BF (b→ sγ) and (g − 2)µ
⋆ Non-universal Higgs scalars
– motivated by SO(10) and SU(5) SUSY GUTs
– allow A-funnel at low tan β; higgsino DM at low m0
– enhanced DD/ ID rates
⋆ DM in models with t− b− τ Yukawa unification (SO(10))
⋆ Mixed wino DM
⋆ Bino-wino co-annihilation (BWCA) DM
⋆ Low M3 mixed higgsino DM
⋆ KKLT mixed moduli/AMSB DM
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Conclusions
⋆ Supersymmetry is very compelling BSM theory
⋆ Irrefragable case for CDM has emerged
⋆ Some reach for SUSY at Tevatron
⋆ Huge reach for SUSY at CERN LHC
⋆ Possible early SUSY discovery at LHC: leptons instead of 6ET
⋆ e+e− LC necessary for precision sparticle spectroscopy
⋆ Direct search for WIMP/axion DM is underway
⋆ Indirect search for WIMP DM via Icecube ν telescope
⋆ Indirect search via γ, p, e+, D detection from galactic core/halo WIMP
annihilations
⋆ Solution of mystery of CDM is near if CDM =lightest SUSY particle!
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