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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
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
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
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
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 5
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!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 6
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!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 7
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!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 8
Gauge coupling evolution
Howie Baer, Oklahoma State University colloquium, April 16, 2009 9
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!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 10
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.
Howie Baer, Oklahoma State University colloquium, April 16, 2009 11
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
Soft term evolution and radiative EWSB
Howie Baer, Oklahoma State University colloquium, April 16, 2009 13
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?
Howie Baer, Oklahoma State University colloquium, April 16, 2009 14
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 15
Dark matter versus dark energy
Howie Baer, Oklahoma State University colloquium, April 16, 2009 16
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 17
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 18
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 19
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 20
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 21
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 22
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 23
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 24
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 25
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 26
Production of sparticles at CERN LHC
Howie Baer, Oklahoma State University colloquium, April 16, 2009 27
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 %)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 28
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 29
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 30
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 31
e+e− → W+
1 W−
1 → (qq′Z1) + (eνeZ1) at linear collider
Howie Baer, Oklahoma State University colloquium, April 16, 2009 32
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 33
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 34
D0 saga with missing ET
Howie Baer, Oklahoma State University colloquium, April 16, 2009 35
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 36
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 37
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 38
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?
Howie Baer, Oklahoma State University colloquium, April 16, 2009 39
Precision sparticle measurements at a e+e− linear collider
Howie Baer, Oklahoma State University colloquium, April 16, 2009 40
Direct detection of SUSY DM
⋆ Direct search via neutralino-nucleon scattering
Howie Baer, Oklahoma State University colloquium, April 16, 2009 41
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 42
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 43
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 44
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)
Howie Baer, Oklahoma State University colloquium, April 16, 2009 45
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 46
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
Howie Baer, Oklahoma State University colloquium, April 16, 2009 47
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!
Howie Baer, Oklahoma State University colloquium, April 16, 2009 48