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.

QuickTime™ and a decompressor

are needed to see this picture.

http://www.physics.wisc.edu/groups/particle-theory/

NPACTheoretical Nuclear, Particle, Astrophysics & Cosmology

SSNuDM, Shanghai, September 2012



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



Standard Model Hidden Sector (DM)

BSM Physics: EFT Framework



EFT: Integrate out heavy DOF & retain only light DOF w/ M <<

Thanks: Adam Ritz

Portals



Thanks: Adam Ritz

Classifying Portals



“dark photons”

Thanks: Adam Ritz

Classifying Portals





! scalar DM

! fermionic DM

Mediator mass

Thanks: Adam Ritz

Classifying Portals



Thanks: Adam Ritz

II. Why the Higgs Portal ?



Higgs Boson Searches QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.







Higgs Boson Searches QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.

SM Higgs?





SM Higgs?

• SM “background” well below new CPV expectations

• New expts: 102 to 103 more sensitive

• CPV needed for BAU?



LEP, Tevatron, & ATLAS Exclusion Non-SM Higgs(es) ?

LHC Observation

Precision Tests

LHC Exclusion

SM Higgs properties ?





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



EWPO: data favor a “light” SM-like Higgs scalar



Tension: EWPO + Direct Searches

What is the BSM Energy Scale ?

Remarkable agreement with EWPO



Agreement w/ SM at ~ 10-3 level: ONP = c / 2



~ 10 TeV generically

Barbieri & Strumia ‘99



Must BSM ~ TeV to maintain a weak scale scalar ?


€

H 0

€

H 0

€

NEW

m2 ~ 2

EWPO: for new interactions coupling to gauge bosons or fermions, BSM >> TeV





€

H 0

€

H 0

€

NEW

m2 ~ 2





€

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 ?


Problem Theory Exp’t

• Inflation

• Dark Energy

• Dark Matter

• Phase transitions



Symmetries & Cosmic History

Standard Model Universe

EW Symmetry Breaking: Higgs ?

New Forces ?

QCD: n+p! nuclei

QCD: q+g! n,p…

Astro: stars, galaxies,..



Symmetries & Cosmic History



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



Scalar Fields & Inflation



New Scalars ?

QCD: n+p! nuclei

QCD: q+g! n,p…

Astro: stars, galaxies,..

• Flatness

• Isotropy

• Homogeneity







Scalar Field: Inflaton

“Slow roll”

Reheat



Scalar Fields & Dark Energy

?

• CDM

• Supernovae

• BAOQuickTime™ and a

decompressorare needed to see this picture.




are needed to see this picture. > 0

Cosmological constant ?

Scalar Field: Quintessence ?



Scalar Fields & the Origin of Matter

?

Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation?




?


Electroweak Phase Transition ? New Scalars




? ?

Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ?






• Rotation curves

• Lensing

• Bullet clusters

Electroweak Phase Transition ? New Scalars




? ?

Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ?






• Rotation curves

• Lensing

• Bullet clusters

Electroweak Phase Transition ? New Scalars: CDM ?


• Inflation

• Dark Energy

• Dark Matter



?

?

?

?


• Inflation

• Dark Energy

• Dark Matter



?

?

?

?

Could experimental discovery of a fundamental scalar point to early universe scalar field dynamics?


• Inflation

• Dark Energy

• Dark Matter



?

?

?

?

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


?

?

?

F

?


Increasing mh

New scalars

Baryogenesis Gravity Waves Scalar DM LHC Searches


?

?

?

F

?


Increasing mh

New scalars


“Strong” 1st order EWPT


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSB


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSBYB : CPV & EW sphalerons

€

Aλ


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSBYB : diffuses into interiors

€

Aλ


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSBYB : diffuses into interiors

Preserve YB

initial

Quench EW sph

TC , Esph, Stunnel F()


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSB

GW Spectra: Q & tEW

F()

Detonation & turbulence



nMSSM

Q

tEW


?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSB

GW Spectra: Q & tEW

F()



?

?

?

F

?


Increasing mh

New scalars



Bubble nucleation

EWSB



?

?

?

F

?


Increasing mh

New scalars

Baryogenesis Gravity Waves Scalar DM ? LHC Searches ?


Bubble nucleation

EWSB

TC , Esph, Stunnel

Q & tEW

F()

YB preservation, detonation & turbulence

Dark Matter: & SI



Thermal DM: WIMP

SM

SM



Direct detection: Spin-indep DM-nucleus scattering



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)



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

⎛

⎝ ⎜

⎞

⎠ ⎟


• 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


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

⎛

⎝ ⎜

⎞

⎠ ⎟





Production Decay

DM Scenario



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


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

⎛

⎝ ⎜

⎞

⎠ ⎟





Production Decay

DM Scenario



DM & SI




are needed to see this picture.+ +…QuickTime™ and a


DM PhenomenologyRelic Density



He, Li, Li, Tandean, Tsai



Direct Detection




Barger, Langacker, McCaskey, R-M, Shaugnessy

HS

S

f

f

-

Higgs pole

LHC & Higgs Phenomenology

LHC discovery potential


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




Invisible decays




Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld ‘00)

Dijet azimuthal distribution

€

h j

€

A

€

A



(h!SS)=0 Invis search



Production Decay




Invisible decays




€

h j

€

A

€

A



Production Decay

Jets + ET

VBF: Invisible Search I

H ! W+W- ! jj : ideally only W decay products in central region (Chehime & Zeppenfeld ‘93)



H ! W+W- ! l + l - : central region minijet from SM bcknd, separation from dilepton pair (Barger, Phillips, Zeppenfeld ‘94)

Central Jet Veto



“Lego plot”

VBF: Invisible Search II





pT (H) distribution



Large pT (invisible decay)

Cahn et al ‘87

VBF + Invis decay

SM bcknd




Invisible decays




€

h j

€

A

€

A



Production Decay



ATLAS




Giardino et al:

arXiv 1207:1347




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







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







HW Question 2

Explain why the scaled direct detection cross section is insensitive to the value of the coupling 2

Complex Singlet: LHC Discovery


Traditional search: CMS





Invisible search: ATLAS

Single component case (x0 = 0)

EWPT

€

h j

€

A

€

A

SM Higgs?



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 ?



He et al



Barger, Langacker, McCaskey, RM, Shaugnessy

EWPT



WIMP-Nucleus Scattering

Viable Dark Matter ?



Gonderinger, Lim, R-M

2nd light state• TH < WMAP

• Xenon

• Br(inv) > 0.6




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


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


New feature: gauge interactions & direct detection


are needed to see this picture. Y = 2 ( Q - I3 )

gZ / 2 I3 - 4 Q sin2 W

Want Y = 0

Real Triplet


New feature: gauge interactions & LHC production

q

q

W +q

q

Z 0

EW cross sections w/ charged states + ET

LHC Phenomenology




Four scalars: h1 (Higgs-like) (dark matter)

(new states)




D

D

€

h j

€

h j

D

D



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





€

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−



Cuts: large ET hard jet One 5cm track

Cirelli et al:



M = 500 GeV:

CDM ~ 0.1

SM Higgs?







Four scalars: h1 (Higgs-like) (dark matter)

(new states)

D

D

€

h j

€

h j

D

D



Fileviez-Perez, Patel, R-M, Wang

€

h j

γ

γ





Real Triplet : H1 Decays

Neutral SM-like Higgs: H+ loops and BR ( H1!γγ)

X0=0: DM case





X0>0: EWPT case

SM Higgs?




LHC: H ! γγ

D

D

€

h j

€

h j

D

D



€

h j

γ

γ









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



J1

J2

V

V

p1

p2

Buckley, R-M JHEP 1109 (2011) 094



R-hadrons from gg fusion

Scalars

Fermions

New Scalars & BSM

Preserving EW Min “Funnel plot”


are needed to see this picture.QuickTime™ and a


VEFF

perturbativity

mH

top loops

naïve stability scale

EW vacuum

Gonderinger, Li, Patel, R-M

SM stability & pert’vity

SM unstable above ~ 8 TeV



top loops sets mH

New Scalars & BSM

Preserving EW Min “Funnel plot”




VEFF

perturbativity

mH

top loops


EW vacuum



top loops


SM stability & pert’vity

SM + singlet: stable but non-pertur’tive

DM-H coupling

Dark Matter StabilityPreserving EW Min



“Funnel plot”





VEFF

perturbativity

mH ?



s

Z2-breaking vacuum

Z2-preserving EW vacuum

No DM: Z2-breaking vac

top loops


EW vacuum

mS2 = b2 + a2 v2

V. Long Range Dark Forces

Torsion Balances & Dark Forces

New interactions in the dark sector ?

€

0

€

€

0 €

0

€

0

• 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




Carroll, Mantry, RM, Stubbs Bovy & Farrar



Kesden & Kamionkowski



Eot-Wash



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




Trigger: Monojet (ISR) + large ET €

qq → W ±* → H ±H2

€

qq → Z*,γ * → H +H−



Cuts: large ET hard jet One 5cm track




€

qq → W ±* → H ±H2

€

qq → Z*,γ * → H +H−



Trigger: Monojet (ISR) + large ET

LHC Phenomenology

Signatures





EWPO compatible

m2 > 2 m1

m1 > 2 m2

LHC: reduced BR(h SM)

€

h1

€

h2

€

h1€

b

€

b

€

γ

€

γ


Production Decay



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

€

h1

€

h2



EWPO comp w/ a1=0=b3



LHC: reduced BR(h SM)



Probing : WBF

H ! ZZ! 4 l

H ! WW! 2j l

• Early LHC discovery possible

• Determine as low as ~ 0.5

DM & Higgs PhenomenologyRelic Density





Direct Detection



Vac stability







LHC & Higgs PhenomenologyVac stab & perturbativity





Invisible decays He, Li, Li, Tandean, Tsai


LHC & Higgs PhenomenologyVac stab & pertubativity





Invisible decays




(h!SS)=0 Invis search




Real Triplet : Charged BRs I

Charged: x0 dependence





€

H ± → H2W±*→ H2π ±

Pure gauge

€

H ± →W ±Z, f1 f 2 x0 suppressed

Real Triplet : Heavy Neutral State

Neutral: differences with SM Higgs & a2 dependence







Different ratio of WW and ZZ, γγ BRs

DM & Higgs PhenomenologyRelic Density





Vac stability



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Scalar Dark Matter and the Higgs Portal