electroweak phase transition, scalar dark matter, & the lhc m.j. ramsey-musolf wisconsin-madison...
TRANSCRIPT
Electroweak Phase Transition, Scalar Dark Matter, & the LHC
M.J. Ramsey-MusolfWisconsin-MadisonQuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
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http://www.physics.wisc.edu/groups/particle-theory/
NPACTheoretical Nuclear, Particle, Astrophysics & Cosmology
TNT Colloquium, November 2012
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Recent Work• M. Gonderinger, Y. Li, H. Patel, & MRM, arXiv:1202.1316
• M. Buckley & MRM JHEP 1109 (2011) 094
• H. Patel & MRM, JHEP 1107 (2011) 029
• C. Wainwright, S. Profumo, MRM Phys Rev. D84 (2011) 023521
• M. Gonderinger, H. Lim, & MRM, Phys. Rev. D86 (2012) 043511
• W. Chao, M. Gonderinger, & MRM, arXiv:1210.0491
Earlier Work
• D. O’Connell, MRM, & M.B. Wise, PR D75 (2007) 037701
• S. Profumo, MRM, & G. Shaugnessy, JHEP 0708 (2007) 010
• V. Barger, P. Langacker, M. McCaskey, MRM, & G. Shaugnessy, PR D77 (2008) 035005, D79 (2009) 015018
• P. Fileviez-Perez, H. Patel, MRM & K. Wang, PR D79 (2009) 055024
Stuart J. Freedman
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Outline
I. Intro & Motivation
II. EWPT & General Features
III. Three minimal extensions of the Standard Model scalar sector
IV. ( How will we know it’s a scalar ? )
V. ( Theoretical issues )
I. Intro & Motivation
Scalar Fields in Cosmology
What role do scalar fields play (if any) in the physics of the early universe ?
Dark Matter Portals
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Standard Model Hidden Sector (DM)
Scalar Fields & the Higgs Portal
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Scalar Fields in Particle Physics
Scalar fields are a simple
Has a fundamental scalar finally been discovered ?
Scalar fields are theoretically problematic
€
H 0
€
H 0
€
ϕ NEW
m2 ~ 2
If so, is it telling us anything about ?
What is the BSM Energy Scale ?
Remarkable agreement with EWPO
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EWPO: data favor a “light” SM-like Higgs scalar
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Tension: EWPO + Direct Searches
What is the BSM Energy Scale ?
Remarkable agreement with EWPO
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Agreement w/ SM at ~ 10-3 level: ONP = c / 2
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~ 10 TeV generically
Barbieri & Strumia ‘99
Scalar Fields in Particle Physics
Scalar fields are a simple
Must BSM ~ TeV to maintain a weak scale scalar ?
Scalar fields are theoretically problematic
€
H 0
€
H 0
€
ϕ NEW
m2 ~ 2
EWPO: for new interactions coupling to gauge bosons or fermions, BSM >> TeV
Scalar Fields in Particle Physics
Scalar fields are a simple
Must BSM ~ TeV to maintain a weak scale scalar ?
Scalar fields are theoretically problematic
€
H 0
€
H 0
€
ϕ NEW
m2 ~ 2
Perhaps new weak scale physics couples only to scalar sector: “Higgs portal”
Scalar Fields in Cosmology
Problem Theory Exp’t
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
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Scalar Fields & Cosmic History
Standard Model Universe
EW Symmetry Breaking: Higgs ?
New Scalars ?
QCD: n+p! nuclei
QCD: q+g! n,p…
Astro: stars, galaxies,..
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Scalar Fields & Inflation
Standard Model Universe
EW Symmetry Breaking: Higgs ?
New Scalars ?
QCD: n+p! nuclei
QCD: q+g! n,p…
Astro: stars, galaxies,..
• Flatness
• Isotropy
• Homogeneity
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Scalar Field: Inflaton
“Slow roll”
Reheat
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Scalar Fields & Dark Energy
?
• CDM
• Supernovae
• BAOQuickTime™ and a
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Cosmological constant ?
Scalar Field: Quintessence ?
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Scalar Fields & the Origin of Matter
?
Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?
• BBN ( t ~ 100 s )
• CMB ( t ~ 105 y )
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Scalar Fields & the Origin of Matter
?
Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?
• BBN ( t ~ 100 s )
• CMB ( t ~ 105 y )
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Electroweak Phase Transition ? New Scalars
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Scalar Fields & the Origin of Matter
? ?
Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ?
Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?
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• Rotation curves
• Lensing
• Bullet clusters
Electroweak Phase Transition ? New Scalars
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Scalar Fields & the Origin of Matter
? ?
Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ?
Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?
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• Rotation curves
• Lensing
• Bullet clusters
Electroweak Phase Transition ? New Scalars: CDM ?
Scalar Fields in Cosmology
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
Problem Theory Exp’t
?
?
?
?
Scalar Fields in Cosmology
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
Problem Theory Exp’t
?
?
?
?
Could experimental discovery of a fundamental scalar point to early universe scalar field dynamics?
Scalar Fields in Cosmology
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
Problem Theory Exp’t
?
?
?
?
Focus of this talk, but perhaps part of larger role of scalar fields in early universe
Questions for this Talk:
• Was there a cosmic phase transition at T ~ 100 GeV ?
• Did it have the characteristics needed for successful electroweak baryogenesis and/or production of gravity waves?
• Are its dynamics coupled to dark matter ?
• What are the experimental signatures ?
• How robust is the underlying theory ?
II. General Features
Effective Potential
L = (D y D - V( )
Tree level
V( ) ) VEFF( ,T)
Quantum corrections
* Many applications: Effective action
*
• T=0 : Coleman-Weinberg (RG improved)
• T>0 : Finite-T effective potential
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSB
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSBYB : CPV & EW sphalerons
€
Aλ
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSBYB : diffuses into interiors
€
Aλ
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSBYB : diffuses into interiors
Preserve YB
initial
Quench EW sph
€
Aλ
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSBYB : diffuses into interiors
Preserve YB
initial
Quench EW sph
TC , Esph, Stunnel F(ϕ)
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSB
Detonation & turbulence
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSB
GW Spectra: Q & tEW
F(ϕ)
Detonation & turbulence
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM LHC Searches
“Strong” 1st order EWPT
Bubble nucleation
EWSB
GW Spectra: Q & tEW
F(ϕ)
Detonation & turbulence
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nMSSM
Q
tEW
EW Phase Transition: New Scalars
?
?
?
F
?
F1st order 2nd order
Increasing mh
New scalars
Baryogenesis Gravity Waves Scalar DM ? LHC Searches ?
“Strong” 1st order EWPT
Bubble nucleation
EWSB
TC , Esph, Stunnel
Q & tEW
F(ϕ)
YB preservation, detonation & turbulence
Higgs Boson Searches QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
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SM Higgs?
• SM “background” well below new CPV expectations
• New expts: 102 to 103 more sensitive
• CPV needed for BAU?
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LEP, Tevatron, & ATLAS Exclusion Non-SM Higgs(es) ?
LHC Observation
Precision Tests
LHC Exclusion
SM Higgs properties ?
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Dark Matter: & SI
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Thermal DM: WIMP
SM
SM
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Direct detection: Spin-indep DM-nucleus scattering
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A
A
III. Simplest Scalar Extensions
Extension EWPT DMDOF
May be low-energy remnants of UV complete theory & illustrative of generic features
Real singlet
Real singlet
Complex Singlet
Real Triplet
1
1
2
3
?
Higgs Portal: Simple Scalar Extensions
Extension EWPT DMDOF
May be low-energy remnants of UV complete theory & illustrative of generic features
Real singlet
Real singlet
Complex Singlet
Real Triplet
1
1
2
3
?
The Simplest Extension
Model
Independent Parameters:
v0, x0, 0, a1, a2, b3, b4
H-S MixingH1 ! H2H2
€
M 2 =μh
2 μhs2 2
μhs2 2 μ s
2
⎛
⎝ ⎜
⎞
⎠ ⎟
Mass matrix
€
h1
h2
⎛
⎝ ⎜
⎞
⎠ ⎟=
sinθ cosθ
cosθ −sinθ
⎛
⎝ ⎜
⎞
⎠ ⎟h
s
⎛
⎝ ⎜
⎞
⎠ ⎟
Stable S (dark matter?)
• Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh
• x0 =0 to prevent h-s mixingxSM EWPT:
Signal Reduction Factor
Production Decay
Simplest extension of the SM scalar sector: add one real scalar S (SM singlet)
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EWPT: a1,2 = 0 & <S> = 0
DM: a1 = 0 & <S> = 0
/ /
O’Connel, R-M, Wise; Profumo, R-M, Shaugnessy; Barger, Langacker, McCaskey, R-M Shaugnessy; He, Li, Li, Tandean, Tsai; Petraki & Kusenko; Gonderinger, Li, Patel, R-M; Cline, Laporte, Yamashita; Ham, Jeong, Oh; Espinosa, Quiros; Konstandin & Ashoorioon…
The Simplest Extension
Model
Independent Parameters:
v0, x0, 0, a1, a2, b3, b4
H-S MixingH1 ! H2H2
€
M 2 =μh
2 μhs2 2
μhs2 2 μ s
2
⎛
⎝ ⎜
⎞
⎠ ⎟
Mass matrix
€
h1
h2
⎛
⎝ ⎜
⎞
⎠ ⎟=
sinθ cosθ
cosθ −sinθ
⎛
⎝ ⎜
⎞
⎠ ⎟h
s
⎛
⎝ ⎜
⎞
⎠ ⎟
Stable S (dark matter?)
• Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh
• x0 =0 to prevent h-s mixingxSM EWPT:
Signal Reduction Factor
Production Decay
EWPT Scenario
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Raise barrier Lower TC : a2 < 0
Finite Temperature Potential
?
?
?
F
?
F
€
H 0
€
S
?
?
?
F
?
F
€
H 0
€
S
Multiple fields & new interactions: novel patters of symmetry breaking, lower TC , greater super-cooling, “stronger 1st order EWPT”
The Simplest Extension
Model
Independent Parameters:
v0, x0, 0, a1, a2, b3, b4
H-S MixingH1 ! H2H2
€
M 2 =μh
2 μhs2 2
μhs2 2 μ s
2
⎛
⎝ ⎜
⎞
⎠ ⎟
Mass matrix
€
h1
h2
⎛
⎝ ⎜
⎞
⎠ ⎟=
sinθ cosθ
cosθ −sinθ
⎛
⎝ ⎜
⎞
⎠ ⎟h
s
⎛
⎝ ⎜
⎞
⎠ ⎟
Stable S (dark matter?)
• Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh
• x0 =0 to prevent h-s mixingxSM EWPT:
Signal Reduction Factor
Production Decay
Low energy phenomenology
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Raise barrier Lower TC
Mixing Modified BRs
Two mixed (singlet-doublet) states w/ reduced SM branching ratios
Mixed States
h1 = cos h + sin s
h2 = -sin h + cos s
EWPT & LHC Phenomenology
Signatures
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m2 > 2 m1
m1 > 2 m2
LHC: reduced BR(h SM)
Signal Reduction Factor
Production Decay
Light: all models Black: LEP allowed
Scan: EWPT-viable model parameters
LHC exotic final states: 4b-jets, + 2 b-jets…
€
h2
€
h1
€
h2
Profumo, R-M, Shaugnessy
€
h1
€
h2
€
h1€
b
€
b
€
€
EWPT & LHC Phenomenology
Signatures
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EWPO compatible
m2 > 2 m1
m1 > 2 m2
LHC: reduced BR(h SM)
Scan: EWPT-viable model parameters
LHC exotic final states: 4b-jets, + 2 b-jets…
Profumo, R-M, Shaugnessy
Signal Reduction Factor
Production Decay
Scan: EWPT-viable model parameters
Light: all models Black: LEP allowed
EWPT & LHC Phenomenology
Signatures
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EWPO compatible
m2 > 2 m1
m1 > 2 m2
LHC: reduced BR(h SM)
Signal Reduction Factor
Production Decay
Light: all models Black: LEP allowed
Scan: EWPT-viable model parameters
LHC exotic final states: 4b-jets, + 2 b-jets…
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EWPO comp w/ a1=0=b3
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LHC: reduced BR(h SM)
Profumo, R-M, Shaugnessy
EWPT & LHC Phenomenology
Signatures
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EWPO compatible
m2 > 2 m1
m1 > 2 m2
LHC: reduced BR(h SM)
Signal Reduction Factor
Production Decay
Light: all models Black: LEP allowed
Scan: EWPT-viable model parameters
LHC exotic final states: 4b-jets, + 2 b-jets…
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EWPO comp w/ a1=0=b3
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LHC: reduced BR(h SM)
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CMS 30 fb-1
SM-like
Singlet-like
SM-like
SM-like w/ H2 ->H1H1 or Singlet-like
Barger, Langacker, McCaskey, R-M, Shaugnessy
The Simplest Extension
Model
Independent Parameters:
v0, x0, 0, a1, a2, b3, b4
H-S MixingH1 ! H2H2
€
M 2 =μh
2 μhs2 2
μhs2 2 μ s
2
⎛
⎝ ⎜
⎞
⎠ ⎟
Mass matrix
€
h1
h2
⎛
⎝ ⎜
⎞
⎠ ⎟=
sinθ cosθ
cosθ −sinθ
⎛
⎝ ⎜
⎞
⎠ ⎟h
s
⎛
⎝ ⎜
⎞
⎠ ⎟
Stable S (dark matter?)
• Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh
• x0 =0 to prevent h-s mixingxSM EWPT:
Signal Reduction Factor
Production Decay
DM Scenario
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DM & SI
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DM PhenomenologyRelic Density
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He, Li, Li, Tandean, Tsai
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Direct Detection
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He, Li, Li, Tandean, Tsai
Barger, Langacker, McCaskey, R-M, Shaugnessy
New Scalars & BSM
Preserving EW Min “Funnel plot”
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VEFF
perturbativity
mH
top loops
naïve stability scale
EW vacuum
Gonderinger, Li, Patel, R-M
SM stability & pert’vity
SM unstable above ~ 108 TeV
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top loops sets mH
New Scalars & BSM
Preserving EW Min “Funnel plot”
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VEFF
perturbativity
mH
top loops
naïve stability scale
EW vacuum
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top loops
Gonderinger, Li, Patel, R-M
SM stability & pert’vity
SM + singlet: stable but non-pertur’tive
DM-H coupling
Dark Matter StabilityPreserving EW Min
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“Funnel plot”
Gonderinger, Li, Patel, R-M
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VEFF
perturbativity
mH ?
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s
Z2-breaking vacuum
Z2-preserving EW vacuum
No DM: Z2-breaking vac
top loops
naïve stability scale
EW vacuum
mS2 = b2 + a2 v2
LHC & Higgs Phenomenology
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Invisible decays
He, Li, Li, Tandean, Tsai
Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)
Dijet azimuthal distribution
€
h j
€
A
€
A
LHC discovery potential
Signal Reduction Factor
Production Decay
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ATLAS
LHC & Higgs Phenomenology
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Giardino et al:
arXiv 1207:1347
Higgs Portal: Simple Scalar Extensions
Extension EWPT DMDOF
May be low-energy remnants of UV complete theory & illustrative of generic features
Real singlet
Real singlet
Complex Singlet
Real Triplet
1
1
2
3
?
Complex Singlet: EWB & DM?
Barger, Langacker, McCaskey, R-M Shaugnessy
Spontaneously & softly broken global U(1)
Controls CDM , TC , & H-S mixing
Gives non-zero MA
Complex Singlet: EWB & DM
Barger, Langacker, McCaskey, R-M, Shaugnessy 2 controls CDM& EWPT
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MH1 = 120 GeV, MH2=250 GeV, x0=100 GeV
decreasing TC
Complex Singlet: EWB & DM?
Barger, Langacker, McCaskey, R-M Shaugnessy
Consequences:
Three scalars: h1 , h2 : mixtures of h & S
A : dark matter
Phenomenology: • Produce h1 , h2 w/ reduced
Reduce BR (hj ! SM)
• Observation of BR (invis)
• Possible obs of SI
Complex Singlet: Direct Detection
Barger, Langacker, McCaskey, R-M, Shaugnessy Two component case (x0=0)
Little sensitivity of scaled SI to
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SM Higgs?
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Three scalars: h1,2 (Higgs-like)
D (dark matter) LHC: WBF “Invisible decay” search
D
D
€
h j
€
h j
D
D
SM Branching Ratios ?
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He et al
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Barger, Langacker, McCaskey, RM, Shaugnessy
EWPT
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WIMP-Nucleus Scattering
Viable Dark Matter ?
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Gonderinger, Lim, R-M
2nd light state• TH < WMAP
• Xenon
• Br(inv) > 0.6
= 1 TeV
Higgs Portal: Simple Scalar Extensions
Extension EWPT DMDOF
May be low-energy remnants of UV complete theory & illustrative of generic features
Real singlet
Real singlet
Complex Singlet
Real Triplet
1
1
2
3
?
Real Triplet
~ ( 1, 3, 0 )
EWPT: a1,2 = 0 & <> = 0
DM & EWPT: a1 = 0 & <> = 0
/ /
Small: -param
Fileviez-Perez, Patel, Wang, R-M: PRD 79: 055024 (2009); 0811.3957 [hep-ph]
Finite Temperature Potential
?
?
?
F
?
F
€
H 0
€
S
Multi-step EWSB transition:
• Step 1: quench sphalerons
• Step 2: move to EW/DM vac
H. Patel & MRM in progress
Real Triplet
~ ( 1, 3, 0 )Fileviez-Perez, Patel, Wang, R-M: 0811.3957 [hep-ph]
New feature: gauge interactions & direct detection
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gZ / 2 I3 - 4 Q sin2 W
Want Y = 0
Real Triplet
~ ( 1, 3, 0 )Fileviez-Perez, Patel, Wang, R-M: 0811.3957 [hep-ph]
New feature: gauge interactions & LHC production
q
q
W +q
q
Z 0
EW cross sections w/ charged states + ET
Real Triplet : DM Search
Basic signature: Charged track disappearing after ~ 5 cm
SM Background: QCD jZ and jW w/ Z ! & W!l
Trigger: Monojet (ISR) + large ET €
qq → W ±* → H ±H2
€
qq → Z*,γ * → H +H−
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Cuts: large ET hard jet One 5cm track
Cirelli et al:
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M = 500 GeV:
CDM ~ 0.1
SM Higgs?
• SM “background” well below new CPV expectations
• New expts: 102 to 103 more sensitive
• CPV needed for BAU?
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SM Branching Ratios ?
Four scalars: h1 (Higgs-like) (dark matter)
(new states)
D
D
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h j
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D
D
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Fileviez-Perez, Patel, R-M, Wang
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h j
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SM Higgs?
• SM “background” well below new CPV expectations
• New expts: 102 to 103 more sensitive
• CPV needed for BAU?
LHC: H !
D
D
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h j
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D
D
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IV. Is it a Scalar ?
Real singlet
Real singlet
Complex Singlet
Real Triplet
Extension EWPT DM
?
DOF
1
1
2
3
IV. Is it a Scalar ?
Real singlet
Real singlet
Complex Singlet
Real Triplet
Extension EWPT DM
?
DOF
1
1
2
3
Mixed Higgs-like states and/or modified BRs: signal reduction invisible search…
IV. Is it a Scalar ?
Real singlet
Real singlet
Complex Singlet
Real Triplet
Extension EWPT DM
?
DOF
1
1
2
3
Could be fermionic triplet [e.g., Buckley, Randall, Shuve, JHEP 1105 (2011) 97]. How to distinguish?
Di-Jet Correlations
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J1
J2
V
V
p1
p2
Buckley, R-M JHEP 1109 (2011) 094
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R-hadrons from gg fusion
Scalars
Fermions
Di-Jet Correlations
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J1
J2
V
V
p1
p2
Buckley, R-M JHEP 1109 (2011) 094
M2
M1
Mpair
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A3 / |Mpair | 2 > 0Scalars:
• Abelian
• Non-ableian for large
Fermions: A3 < 0
V. Theoretical Issues
Gauge-dependence in VEFF ( , T )
VEFF ( , T ) ! VEFF ( , T ; )
Ongoing research: approaches for carrying out tractable, GI computations
• H. Patel & MRM, JHEP 1107 (2011) 029
• C. Wainwright, S. Profumo, MRM Phys Rev. D84 (2011) 023521
• H. Gonderinger, H. Lim, & MRM, arXiv:1202.1316
Origin of Gauge Dependence
Effective Action
Effective Potential
Source term:
Not GI
Nielsen Identities
Identity:
Extremal configurations:
Effective potential:
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Baryon Number Preservation “Washout factor”
F()
ln S ~ A(TC) e
Two qtys of interest:
• TC from Veff
• Esph from eff
Baryon Number Preservation: Pert Theory
~
F()
Conventional treatments
Gauge Dep
• GI TC from hbar exp, Veff (ϕϕ), or Hamiltonian formulation
• Use GI scale in Esph computation
H. Patel & MRM, JHEP 1107 (2011) 029“Baryon number preservation criterion” (BNPC)
Nielsen Identities: Application to TC
Critical Temperature
Veff (min , TC) = Veff ( , TC)
Apply consistently order-by-order in
Implement minimization order-by-order (defines ϕn )
Fukuda & Kugo ‘74: T=0 VEFF
Laine ‘95 : 3D high-T Eff Theory
Patel & R-M ‘11: Full high T Theory
Obtaining a GI TC
Track evolution of minima with T using expansion
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Track evolution of different minima with T using
n=1
n=2 n=3
Patel & R-M ‘11
Illustrative results in SM:
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Full ϕ
Gravity Waves from EWPT: Pert Theory
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Abelian Higgs Model
C. Wainwright, S. Profumo, R-M Phys Rev. D84 (2011) 023521 arXiv:1104.5487[hep-ph]
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Vacuum Stability & Gauge DependenceComplex Singlet Model
M. Gonderinger, H. Lim, M. R-M arXiv:1202.1316 [hep-ph]
?
?
?
F
?
F
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H 0
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S
Possible runaway direction for 2 < 0 (EWPT)
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Tree-level stability
Full VEFF (1-loop): -dependence
GI Stability Condition
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Use -fns
Conclusions
• Cosmology loves scalar fields (inflation): given observation of a fundamental scalar, perhaps scalar fields can address a number of questions about the early universe
• Simple extensions of the SM scalar sector and lead to observable (SI , LHC) particle dark matter and/or EWPT with interesting implications: baryogenesis, GW, new Higgs states/modified Higgs properties….
• Perhaps observation of these scalars will point to a richer structure for scalar fields in the early universe involving both visible and dark physics
Back Up Slides
LHC & Higgs Phenomenology
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Invisible decays
He, Li, Li, Tandean, Tsai
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Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)
Dijet azimuthal distribution
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h j
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A
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A
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(h!SS)=0 Invis search
LHC discovery potential
Signal Reduction Factor
Production Decay
LHC & Higgs Phenomenology
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Invisible decays
He, Li, Li, Tandean, Tsai
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Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)
Dijet azimuthal distribution
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A
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A
LHC discovery potential
Signal Reduction Factor
Production Decay
Complex Singlet: LHC Discovery
Barger, Langacker, McCaskey, R-M, Shaugnessy
Traditional search: CMS
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Invisible search: ATLAS
Single component case (x0 = 0)
EWPT
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A
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Baryon Number Preservation: Pert Theory
~
F()
Conventional treatments
“Baryon number preservation criterion” (BNPC)
DM & Higgs PhenomenologyRelic Density
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Vac stability
He, Li, Li, Tandean, Tsai
Gonderinger, Li, Patel, R-M
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A
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Nielsen Identities: Example
General SU(N) theory:General SU(N) theory:
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Scalars: physical & WB GB
T & L gauge bosons
Scalar gauge bosons
FP Ghosts
Use ϕ0 : mA2(ϕ0)ij & Mij
2(ϕ0) simultaneously diagonalizable & eigenvalues in distinct subspaces ! -dependent WB GB, scalar gauge, & FPG terms cancel
Patel & R-M ‘11
Scalar Fields in Cosmology
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
Problem Theory Exp’t
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Scalar Fields & Cosmic History
Standard Model Universe
EW Symmetry Breaking: Higgs ?
New Forces ?
QCD: n+p! nuclei
QCD: q+g! n,p…
Astro: stars, galaxies,..
BBN and YB
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CMB and YB
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Cosmic Baryon Asymmetry
?
Baryogenesis: When? CPV? SUSY? Neutrinos?
Big Bang Nucleosynthesis:
Light element abundances depend on YB
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Cosmic Baryon Asymmetry
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Baryogenesis: When? CPV? SUSY? Neutrinos?
Cosmic Microwave Bcknd:
Shape of anisotropies depends on YB
VBF: Invisible Search I
Central Jet Veto
H ! W+W- ! jj : ideally only W decay products in central region (Chehime & Zeppenfeld ‘93)
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H ! W+W- ! l + l - : central region minijet from SM bcknd, separation from dilepton pair (Barger, Phillips, Zeppenfeld ‘94)
VBF: Invisible Search II
pT (H) distribution
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Large pT (invisible decay)
Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)
Dijet azimuthal distribution
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ϕ
Cahn et al ‘87
Complex Singlet: EWB & DM?
Barger, Langacker, McCaskey, R-M Shaugnessy
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Key features for EWPT & DM: (1) Softly broken global U(1)
(2) Closes under renormalization
(3) SSB leading to two fields: S that mixes w/ h and A is stable (DM)
Complex Singlet: EWB & DM?
Barger, Langacker, McCaskey, R-M Shaugnessy
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Key features for EWPT & DM: (1) Softly broken global U(1)
(2) Closes under renormalization
(3) SSB leading to two fields: S that mixes w/ h and A is stable (DM)
Controls CDM& EWPT
Normalized Latent Heat
Peak amplitude:
GW Spectra (detonations):
Peak frequency:
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See, eg, Caprini, Durrer, Servant ‘08; Huber & Konstandin ‘08; Caprini et al ‘09; Chung & Zhou ‘10