Chiral Symmetries and Low Energy Searches for New Physics
M.J. Ramsey-Musolf
CaltechWisconsin-Madison
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Fundamental Symmetries & Cosmic History
• What were the fundamental symmetries that governed the microphysics of the early universe?
• Were there additional (broken) chiral symmetries?
• What insights can low energy (E << MZ) precision electroweak studies provide?
• How does the approximate chiral symmetry of QCD the affect low energy search for newsymmetries?
Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Puzzles the Standard Model can’t solve
1. Origin of matter2. Unification & gravity
3. Weak scale stability4. Neutrinos
What are the symmetries (forces) of the early universe beyond those of the SM?
What are the new fundamental symmetries?
Two frontiers in the search
Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ)
Indirect searches at lower energies (E < MZ) but high precision
High energy physics
Particle, nuclear & atomic physics
CERN
Ultra cold neutronsLarge Hadron Collider
LANSCE, NIST, SNS, ILL
What are the new fundamental symmetries?
• Why is there more matter than antimatter in the present universe?
• What are the unseen forces that disappeared from view as the universe cooled?
• What are the masses of neutrinos and how have they shaped the evolution of the universe?
Electric dipole moment & dark matter searches
Precision electroweak: weak decays & e- scattering
Neutrino interactions & 0-decayTribble report
Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Cosmic Energy Budget
?
Baryogenesis: When? SUSY? Neutrinos? CPV?
WIMPy D.M.: Related to baryogenesis?
“New gravity”? Grav baryogenesis?
Weak scale baryogenesis can be tested experimentally
What is the origin of baryonic matter ?
Cosmic Energy Budget
Baryons
Dark Matter
Dark Energy
Searches for permanent electric dipole moments (EDMs) of the neutron, electron, and neutral atoms probe new CP-violation
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rE
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rd = d
r S
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EDM = −d
r S ⋅
r E
h
T-odd , CP-odd by CPT theorem
What are the quantitative implications of new EDM experiments for explaining the origin of the baryonic component of the Universe ?
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YB =ρ B
sγ
=(7.3± 2.5) ×10−11
(9.2 ±1.1) ×10−11
BBN
WMAP
Chiral odd SU(2)L x U(1)Y invariant for >> Mweak
SM CPV Yukawa suppressedBeyond SM CPV may not be (e.g., SUSY)
EDM Probes of New CP Violation
f dSM dexp dfuture
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e−
n199Hg
μ
< 10−40
< 10−30
< 10−33
< 10−28
< 1.6 ×10−27
< 3.0 ×10−26
< 2.1×10−28
< 1.1×10−18
→ 10−31
→ 10−29
→ 10−32
→ 10−24
CKM
If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM?
Also 225Ra, 129Xe, d
Baryogenesis: New Electroweak Physics
Weak Scale Baryogenesis
• B violation
• C & CP violation
• Nonequilibrium dynamics
Sakharov, 1967
?
ϕ new
?
φ(x)
Unbroken phase
Broken phaseCP Violation
Topological transitions
1st order phase transition
?
γ
?
e -?
ψnew• Is it viable?• Can experiment constrain it?• How reliably can we compute it?
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ϕ new
?
ϕ new
90’s: Cohen, Kaplan, Nelson Joyce, Prokopec, Turok
Theoretical Issues:Transport at phase boundary (non-eq QFT)Bubble dynamics (numerical)Strength of phase transition (Higgs sector)EDMs: many-body physics & QCD
Scale Hierarchy: Expand in energy & time scale ratios
Cirigliano, Lee, R-M
Baryogenesis & Dark Matter: SUSY
Supersymmetry
eL,R , qL,R
W,Z,γ,g
˜ W , ˜ Z ,˜ γ , ˜ H u,d ⇒ ˜ χ ±, ˜ χ 0Charginos, neutralinos
Fermions Bosons
˜ e L,R , ˜ q L,R sfermions
˜ W , ˜ Z ,˜ γ , ˜ g gauginos
˜ H u,˜ H dHiggsinos
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Hu,Hd
Baryogenesis & Dark Matter: SUSY
Neutralino Mass Matrix
M1
-
M2
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin W 0
0
0
0
-
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin WMN =
Chargino Mass Matrix
M2
MC =
cos2mW
sin2mWT << TEW : mixing
of H,W to ~ ~ ~ ~
T ~TEW : scattering
of H,W from
background field
~~
?
ϕ new
?
φ(x)
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q , ˜ W , ˜ B , ˜ H u,d
T ~ TEW
CPV
B W Hd Hu
BINO WINO HIGGSINO
T << TEW
EDM constraints & SUSY CPV
AMSB: M1 ~ 3M2
Neutralino-driven baryogenesis
Baryogenesis
LEP II Exclusion
Two loop de
Cirigliano, Profumo, R-M
SUGRA: M2 ~ 2M1
| sin ϕ | > 0.02
| de , dn | > 10-28 e-cm
M < 1 TeV
Precision Ewk Probes of New Symmetries
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Unseen Forces: Supersymmetry ?
1. Unification & gravity2. Weak scale stability
3. Origin of matter4. Neutrinos
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˜ χ 0
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˜ μ −
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˜ ν μ
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Weak decays & new physics
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u c t( )
Vud Vus Vub
Vcd Vcs Vcb
Vtd Vts Vtb
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⎜ ⎜ ⎜
⎞
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n → p e− ν e
A(Z,N) → A(Z −1,N +1) e+ ν e
π + → π 0 e+ ν e
-decay €
d → u e− ν e
s → u e− ν e
b → u e− ν e
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GFβ
GFμ
= Vud 1+ Δrβ − Δrμ( )
New physics
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˜ χ 0
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˜ μ −
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˜ ν μ
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W −
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˜ χ 0
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˜ χ −
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˜ ν μ
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˜ ν e
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+L
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+LSUSY€
δOSUSY
OSM~ 0.001
Flavor-blind SUSY-breaking
CKM, (g-2) MW, Mt ,…
M˜ μ L >M˜ q LKurylov, R-M
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+L
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+LRPV
μ−
ν e e−
νμ
˜ e Rk
12k 12k
e−
d e−
d
˜ q Lj
1j1
1j1
No long-lived LSP or SUSY DM
MW
R Parity Violation
CKM Unitarity
APV
l2
Kurylov, R-M, Su
CKM unitarity ?
See Moulson, Cirigliano
Weak decays & SUSY
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u c t( )
Vud Vus Vub
Vcd Vcs Vcb
Vtd Vts Vtb
⎛
⎝
⎜ ⎜ ⎜
⎞
⎠
⎟ ⎟ ⎟
d
s
b
⎛
⎝
⎜ ⎜ ⎜
⎞
⎠
⎟ ⎟ ⎟
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d → u e− ν e
s → u e− ν e
b → u e− ν e
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−
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˜ χ 0
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˜ μ −
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˜ ν μ
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e
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W −
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u
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˜ χ 0
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˜ u
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˜ ν e
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+L
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+LSUSY€
δOSUSY
OSM~ 0.001
Correlations
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dW ∝1 + ar p e ⋅
r p ν
Ee Eν
+ Ar σ n ⋅
r p eEe
+ L
Non (V-A) x (V-A) interactions: me/E
-decay at SNS,“RIAcino”?
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B me Ee( )r σ n ⋅
r p νEν
+ L
Weak decays & SUSY : Correlations
SUSY loop-induced operators
with mixing between L,R chiral supermultiplets
Yukawa suppressed L-R mixing: “alignment” models
Large L-R mixing: New models for SUSY-breaking
Future exp’t ?
Profumo, R-M, Tulin
Pion leptonic decay & SUSY
A non-zero NEW would shift F
SM radiative corrections important for precise F Holstein, Marciano & Sirlin
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γ
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l
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+L
RPV SUSY
Pion leptonic decay & SUSY
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γ
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l
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+LLeading QCD uncertainty:
Marciano & Sirlin
Probing Slepton Universality
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e−
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˜ χ 0
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˜ u
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˜ ν μvs
New TRIUMF, PSI
Min (GeV)
Tulin, Su, R-M Prelim
Can we do better on ?
Lepton Scattering & New Symmetries
Parity-Violating electron scattering
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ALR =GFQ2
4 2παQW + F(Q2,θ)[ ]
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e−
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e−, p
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Z 0
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γ
“Weak Charge” ~ 1 - 4 sin2 W ~ 0.1
Probing SUSY with PV eN Interactions
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SUSY loops
Kurylov, Su, MR-M
is Majorana
RPV 95% CL fit to weak decays, MW, etc.
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˜ e −
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˜ e +
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δQWe,SUSY QW
e,SMμ−
ν e e−
νμ
˜ e Rk
12k 12k
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δQWp,SUSY QW
p,SM
SUSY dark matter
Probing SUSY with PV eN Interactions
QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
SUSY dark matter
Kurylov, R-M, Su
SUSY loops
RPV 95% CL€
δQWp,SUSY QW
p,SM
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δQWe,SUSY QW
e,SM
E158 &Q-Weak
JLab Moller
Linear collider
“DIS Parity”
SUSY dark matter
Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Neutrinos ?
Are they their own antiparticles?
Why are their masses so small?
Can they have magnetic moments?
Implications of m for neutrino interactions ?
LFV & LNV ?
Neutrino Mass & Magnetic Moments
How large is ?
Experiment: < (10-10 - 10-12) B
e scattering, astro limits
Radiatively-induced m
< 10-14 B Dirac
e < 10-9-10-12 B Majorana
Bell, Cirigliano, Gorshteyn,R-M, Vogel, Wang, Wise Davidson, Gorbahn, Santamaria
Both operators chiral odd
Correlations in Muon Decay & m
Model Independent Analysis
constrained by m
Model Dependent Analysis
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W1,2−
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MWR (GeV )
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TWIST ρ
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TWIST Pμξ
First row CKM
2005 Global fit: Gagliardi et al.
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H 0
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H 0
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H 0
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Z,W
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H 0
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Prezeau, Kurylov 05 Erwin, Kile, Peng, R-M 06 m
MPs
Also -decay, Higgs production
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e−
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e+€
Constraints on non-SM Higgs production at ILC:
m , and decay corr
Neutrino Mass & - decay
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e−
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M
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W −
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W −
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u
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u
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d
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d
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e−
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e−
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0
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˜ e −
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u
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u
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d
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d
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˜ e −
How do we compute & separate heavy particle exchange effects?
Light M : 0-decay rate may yield scale of m
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mν
EFF= Uek
2mk e2iδ
k
∑
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e−
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e−
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A Z,N( )
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A Z + 2,N − 2( )
Neutrino Mass & - decay
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e−
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e−
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M
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W −
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W −
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u
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u
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d
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d
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e−
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0
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˜ e −
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u
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u
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d
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d
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˜ e −
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e−
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A Z,N( )
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A Z + 2,N − 2( )€
u
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d€
u
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d
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e−
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e−
4 quark operator: low energy EFT
How do we compute & separate heavy particle exchange effects?
Neutrino Mass & - decay
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N
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N€
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e−
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e−
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N
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KNNNN p0
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KπNN p−1
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Kππ p−2
Prezeau, R-M, & VogelL(q,e) =
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GF2
Λββ
C j (μ) ˆ O j++ e Γ je
c + h.c.j=1
14
∑
Chiral properties of Oj++
determine p-dependence of K KNN , KNNNN
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ˆ O 1+++ ∈ (3L , 3R ) K ~ O (p0)
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ˆ O 3+++ ∈ (5, 1)⊕ (1, 5) K ~ O (p2)
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e−
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e−
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0
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˜ e −
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u
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u
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d
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d
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˜ e −
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ˆ O 1+++ ∈ (3L , 3R )
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ˆ O 3+++ ∈ (5L , 1R )⊕ (1L , 5R )
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ˆ O 1+++ ∈ (3L , 3R )
No WR - WL
mixing
WR - WL mix
RPV SUSY
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W −
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W −
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u
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u
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d
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d
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e−
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e−
Conclusions
• Low energy probes of physics beyond the SM give us a unique window on the fundamental symmetries of the early universe that complements direct searches for new physics at colliders
•These symmetries - including broken chiral symmetries - are needed to explain the origin of matter, provide for stability of the electroweak scale, incorporate new forces implied by unification, and account for the properties of neutrinos
• The broken chiral symmetry of QCD also provides an important tool for sharpening Standard Model predictions for low energy observables and making any deviations interpretable in terms of new symmetries