Scalar Dark Matter and the Higgs Portal
description
Transcript of Scalar Dark Matter and the Higgs Portal
Scalar Dark Matter and the Higgs Portal
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
SSNuDM, Shanghai, September 2012
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Outline
1. Dark Matter Portals
2. Why the Higgs portal?
3. Why scalar dark matter ?
4. Simplest examples: scalar DM & LHC
5. Long-range dark forces
• Supersymmetry as an illustration
• Theoretical progress & challenges
• Our work
I. Dark Matter Portals
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Standard Model Hidden Sector (DM)
BSM Physics: EFT Framework
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EFT: Integrate out heavy DOF & retain only light DOF w/ M <<
Thanks: Adam Ritz
Portals
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Thanks: Adam Ritz
Classifying Portals
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“dark photons”
Thanks: Adam Ritz
Classifying Portals
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! scalar DM
! fermionic DM
Mediator mass
Thanks: Adam Ritz
Classifying Portals
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Thanks: Adam Ritz
II. Why the Higgs Portal ?
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Higgs Boson Searches QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
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Higgs Boson Searches QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
SM Higgs?
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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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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
€
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
€
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
€
NEW
m2 ~ 2
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
€
NEW
m2 ~ 2
Perhaps new weak scale physics couples only to scalar sector: “Higgs portal”
III. Why scalar dark matter ?
?
Scalar Fields & Early Universe
Scalar Fields in Cosmology
What role do scalar fields play (if any) in the physics of the early universe ?
Scalar Fields in Cosmology
Problem Theory Exp’t
• Inflation
• Dark Energy
• Dark Matter
• Phase transitions
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Symmetries & Cosmic History
Standard Model Universe
EW Symmetry Breaking: Higgs ?
New Forces ?
QCD: n+p! nuclei
QCD: q+g! n,p…
Astro: stars, galaxies,..
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Symmetries & Cosmic History
Standard Model Universe
EW Symmetry Breaking: Higgs ?
New Forces ?
Puzzles the Standard Model can’t solve
1. Origin of matter2. Unification & gravity
3. Weak scale stability4. Neutrinos
SUSY ?
GUTS ?
Extra Dims ? WR
WL*
WL
~
NR
Terascale
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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?
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Scalar Fields & the Origin of Matter
?
Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?
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
Electroweak Phase Transition
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
TC , Esph, Stunnel F()
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()
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
GW Spectra: Q & tEW
F()
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
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
TC , Esph, Stunnel
Q & tEW
F()
YB preservation, detonation & turbulence
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
?
IV. Simple examples
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, Cont’d
€
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=0 to prevent s-h mixing and one-loop s hh
• x0 =0 to prevent h-s mixing & s ! hh
x0 = <S>
€
γ
€
γ h1,2
€
b
€
b
€
γ
€
γ
S
h
h
The Simplest Extension
Model
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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HW Question 1
Consider the real singlet extension: explain why the presence of an operator S3 in addition to H+H S2 would imply that S can decay to Standard Model particles
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
HS
S
f
f
-
Higgs pole
LHC & Higgs Phenomenology
LHC discovery potential
Signal Reduction Factor
Production Decay
V1j < 1: mixed states hj New decays: h2 ! h1 h1
Dark matter: no mixing ! states are h,S
New decays h! SS (invisible!) possible
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
€
h j
€
A
€
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
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
Jets + ET
VBF: Invisible Search I
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)
Central Jet Veto
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“Lego plot”
VBF: Invisible Search II
Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)
Dijet azimuthal distribution
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pT (H) distribution
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Large pT (invisible decay)
Cahn et al ‘87
VBF + Invis decay
SM bcknd
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
< S > = 0
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: 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: Direct Detection
Barger, Langacker, McCaskey, R-M, Shaugnessy Two component case (x0=0)
Little sensitivity of scaled SI to
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HW Question 2
Explain why the scaled direct detection cross section is insensitive to the value of the coupling 2
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
€
h j
€
A
€
A
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
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 )Fileviez-Perez, Patel, Wang, R-M: PRD 79: 055024 (2009); 0811.3957 [hep-ph]
EWPT: a1,2 = 0 & <> = 0
DM & EWPT: a1 = 0 & <> = 0
/ /
Real Triplet
~ ( 1, 3, 0 )Fileviez-Perez, Patel, Wang, R-M: 0811.3957 [hep-ph]
EWPT: a1,2 = 0 & <> = 0
DM & EWPT: a1 = 0 & <> = 0
/ /
Small: -param
Real Triplet
~ ( 1, 3, 0 )Fileviez-Perez, Patel, Wang, R-M: 0811.3957 [hep-ph]
EWPT: a1,2 = 0 & <> = 0
DM & EWPT: a1 = 0 & <> = 0
/ /
Small: -param
HW Question 3
Consider the real triplet extension in which there is no H0 - mixing: explain why cannot decay to Standard Model fermions, unlike the H0
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
LHC Phenomenology
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SM Branching Ratios ?
Four scalars: h1 (Higgs-like) (dark matter)
(new states)
• SM “background” well below new CPV expectations
• New expts: 102 to 103 more sensitive
• CPV needed for BAU?
D
D
€
h j
€
h j
D
D
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Fileviez-Perez, Patel, R-M, Wang
LEP: M > 100 GeV !
BR(invis) = 0
Real Triplet : Charged BRs
Charged: x0 dependence
Below WZ Threshold
Above WZ Threshold
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€
H ± → H2W±*→ H2π ±
Pure gauge
€
H ± →W ±Z, f1 f 2 x0 supressed
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
€
h j
€
h j
D
D
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Fileviez-Perez, Patel, R-M, Wang
€
h j
γ
γ
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Real Triplet : H1 Decays
Neutral SM-like Higgs: H+ loops and BR ( H1!γγ)
X0=0: DM case
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X0>0: EWPT case
SM Higgs?
• SM “background” well below new CPV expectations
• New expts: 102 to 103 more sensitive
• CPV needed for BAU?
LHC: H ! γγ
D
D
€
h j
€
h j
D
D
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€
h j
γ
γ
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Is it a Scalar ?
Real singlet
Real singlet
Complex Singlet
Real Triplet
Extension EWPT DM
?
DOF
1
1
2
3
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…
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
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 ~ 8 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
V. Long Range Dark Forces
Torsion Balances & Dark Forces
New interactions in the dark sector ?
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• Long-range, non-grav dark force
• Violation of weak equiv principle (WEP)• Galactic tidal streams & CMB • New hierarchy problem
Non-sterile DM & terrestrial WEP tests
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Carroll, Mantry, RM, Stubbs Bovy & Farrar
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Kesden & Kamionkowski
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Eot-Wash
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Microscope
Summary
• There exist a number of interesting and viable “portals” for probing the dark sector
• The Higgs portal is particularly interesting now in light of the LHC discovery, and it raises many new questions
• Discovering scalar dark matter via the Higgs portal could make the idea of scalar fields in the early universe more plausible
• Simple scalar sector extensions that embody features of UV complete theories illustrate key features of the theory and phenomenology of scalar dark matter ! A rich and exciting period of experiment and theory lies ahead
Back Up Slides
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
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qq → Z*,γ * → H +H−
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Cuts: large ET hard jet One 5cm track
Real Triplet : DM Search
Basic signature: Charged track disappearing after ~ 5 cm
SM Background: QCD jZ and jW w/ Z !& W!l
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qq → W ±* → H ±H2
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qq → Z*,γ * → H +H−
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Trigger: Monojet (ISR) + large ET
LHC Phenomenology
Signatures
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EWPO compatible
m2 > 2 m1
m1 > 2 m2
LHC: reduced BR(h SM)
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h1
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h2
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h1€
b
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γ
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Signal Reduction Factor
Production Decay
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CMS 30 fb-1
SM-like
Singlet-like
SM-like
SM-like w/ H2 ->H1H1 or Singlet-like
~ EWB Viable
Light: all models Black: LEP allowed
Scan: EWPT-viable model parameters
LHC exotic final states: 4b-jets, γγ + 2 b-jets…€
h2
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h1
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h2
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EWPO comp w/ a1=0=b3
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LHC: reduced BR(h SM)
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Probing : WBF
H ! ZZ! 4 l
H ! WW! 2j l
• Early LHC discovery possible
• Determine as low as ~ 0.5
DM & Higgs PhenomenologyRelic Density
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Direct Detection
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Vac stability
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He, Li, Li, Tandean, Tsai
Gonderinger, Li, Patel, R-M
He, Li, Li, Tandean, Tsai
Barger, Langacker, McCaskey, R-M, Shaugnessy
LHC & Higgs PhenomenologyVac stab & perturbativity
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Invisible decays He, Li, Li, Tandean, Tsai
Gonderinger, Li, Patel, R-M
LHC & Higgs PhenomenologyVac stab & pertubativity
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Invisible decays
LHC discovery potential
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(h!SS)=0 Invis search
He, Li, Li, Tandean, Tsai
Gonderinger, Li, Patel, R-M
Barger, Langacker, McCaskey, R-M, Shaugnessy
Real Triplet : Charged BRs I
Charged: x0 dependence
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H ± → H2W±*→ H2π ±
Pure gauge
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H ± →W ±Z, f1 f 2 x0 suppressed
Real Triplet : Heavy Neutral State
Neutral: differences with SM Higgs & a2 dependence
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Different ratio of WW and ZZ, γγ BRs
DM & Higgs PhenomenologyRelic Density
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Vac stability
He, Li, Li, Tandean, Tsai
Gonderinger, Li, Patel, R-M