Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

An Inverted Mass Hierarchy for ExcitingDark Matter

Andrew R. Frey

McGill University

0901.4327 and work in progresswith Fang Chen and Jim Cline

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

Outline

1 Hints About Dark Matter?

2 The Need for Boost Factors

3 An Inverted Model of Dark Matter

4 Future Directions

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

Hints About Dark Matter?

(Chandra, Hubble, Magellan)

Some Observations

Direct detection

Seen at DAMA, not others?Inelastic scattering?

High energy e± in astrophysics

PAMELA, ATIC, & otherobservationsWMAP haze from synchotronTeV scale DM decays orannihilations?Alternately pulsars

511 keV photon line

INTEGRAL and older (40 yrs!)Strong bulge componentDM decays or transitions?

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

Hints About Dark Matter?

(Chandra, Hubble, Magellan)

Some Observations

Direct detection

Seen at DAMA, not others?Inelastic scattering?

High energy e± in astrophysics

PAMELA, ATIC, & otherobservationsWMAP haze from synchotronTeV scale DM decays orannihilations?Alternately pulsars

511 keV photon line

INTEGRAL and older (40 yrs!)Strong bulge componentDM decays or transitions?

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

Direct Detection

DAMA vs Others

Collisions with nuclei

Only seen at DAMA expts(possible candidates at others)

Main difference = heavy nuclei

Inelastic scattering favors heavy targets

δM . µv2/2

Need δM . 100 keV

But...

DAMA somewhat controversial

I’ll remain agnostic

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

Direct Detection

DAMA vs Others

Collisions with nuclei

Only seen at DAMA expts(possible candidates at others)

Main difference = heavy nuclei

Inelastic scattering favors heavy targets

δM . µv2/2

Need δM . 100 keV

But...

DAMA somewhat controversial

I’ll remain agnostic

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(PAMELA)

(ATIC)

PAMELA

Excess e+ fraction above 10 GeVPossibly:

Pulsars100+ GeV DM Decay τ∼1026 sDM Annihilation σ∼100×WIMPy(leptophilic b/c no excess p̄)

ATIC/PPB-BETS, etc

Excess e± at 100-800 GeV

Distinct peak

Consistent with PAMELA

Similar explanations

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(PAMELA)

(ATIC)

PAMELA

Excess e+ fraction above 10 GeVPossibly:

Pulsars100+ GeV DM Decay τ∼1026 sDM Annihilation σ∼100×WIMPy(leptophilic b/c no excess p̄)

ATIC/PPB-BETS, etc

Excess e± at 100-800 GeV

Distinct peak

Consistent with PAMELA

Similar explanations

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(PAMELA)

(ATIC)

PAMELA

Excess e+ fraction above 10 GeVPossibly:

Pulsars100+ GeV DM Decay τ∼1026 sDM Annihilation σ∼100×WIMPy(leptophilic b/c no excess p̄)

ATIC/PPB-BETS, etc

Excess e± at 100-800 GeV

Distinct peak

Consistent with PAMELA

Similar explanations

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(Finkbeiner et al from WMAP data)

WMAP Haze

Excess microwaves at galaxy center(other foregrounds subtracted)

Synchotron of high energy e±

Consistent with DM annihilation

All require 100- to 1000-fold boost in cross-section forannihilation

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(Finkbeiner et al from WMAP data)

WMAP Haze

Excess microwaves at galaxy center(other foregrounds subtracted)

Synchotron of high energy e±

Consistent with DM annihilation

All require 100- to 1000-fold boost in cross-section forannihilation

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

High Energy e±

(Finkbeiner et al from WMAP data)

WMAP Haze

Excess microwaves at galaxy center(other foregrounds subtracted)

Synchotron of high energy e±

Consistent with DM annihilation

All require 100- to 1000-fold boost in cross-section forannihilation

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

511 keV Line

Observed for almost 4 decades

(INTEGRAL/SPI )

INTEGRAL

e± annihilation nearly at rest

Dominant bulge component

Possibly:

Super-/Hyper-/Novae (e+

escape?)Light DM annihilation (cusps?)Exciting DM

eXciting Dark Matter

DM with 2 states δM & 2me

Requires boosted cross-section

Variant spectra allowed

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

511 keV Line

Observed for almost 4 decades

(INTEGRAL/SPI )

INTEGRAL

e± annihilation nearly at rest

Dominant bulge component

Possibly:

Super-/Hyper-/Novae (e+

escape?)Light DM annihilation (cusps?)Exciting DM

eXciting Dark Matter

DM with 2 states δM & 2me

Requires boosted cross-section

Variant spectra allowed

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

A Sketch of Particle Physics

Non-Abelian symmetry breaking key (Arkani-Hamed et al)

Leptophilia

Gauge bosons naturally lighter

Kinetic mixing with photon

εBµνFµν

Resonant production at µ . 1 GeVdecays to e±

Mass Splittings

Generated at 1-loop

δM ∼ αµ

Naturally MeV , possibly 100 keV

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

A Sketch of Particle Physics

Non-Abelian symmetry breaking key (Arkani-Hamed et al)

Leptophilia

Gauge bosons naturally lighter

Kinetic mixing with photon

εBµνFµν

Resonant production at µ . 1 GeVdecays to e±

Mass Splittings

Generated at 1-loop

δM ∼ αµ

Naturally MeV , possibly 100 keV

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

A Sketch of Particle Physics

Boost Factors

Uncertainty in DM density profile

flux ∼ n2〈σv〉

Or attraction of DM by gauge forces(Sommerfeld enhancement)

Putting It Together

Production of e± only through light bosons

XDM: MeV scale mass splitting through 1-loop

iDM: 100 keV scale splitting through small 1-loop

Not as reliant on hopes for DM clumping to boost

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

A Sketch of Particle Physics

Boost Factors

Uncertainty in DM density profile

flux ∼ n2〈σv〉

Or attraction of DM by gauge forces(Sommerfeld enhancement)

Putting It Together

Production of e± only through light bosons

XDM: MeV scale mass splitting through 1-loop

iDM: 100 keV scale splitting through small 1-loop

Not as reliant on hopes for DM clumping to boost

Inverted XDM

ARF

Outline

DM Hints

Direct Detection

High-E e

511 keV Line

Particle Physics

Boost Factors

Model

Future

A Sketch of Particle Physics

Boost Factors

Uncertainty in DM density profile

flux ∼ n2〈σv〉

Or attraction of DM by gauge forces(Sommerfeld enhancement)

Putting It Together

Production of e± only through light bosons

XDM: MeV scale mass splitting through 1-loop

iDM: 100 keV scale splitting through small 1-loop

Not as reliant on hopes for DM clumping to boost

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

The Need for Boost Factors

Annihilation Case

Early universe cross-section (v ∼ 0.2)

〈σv〉 ∼ 3× 10−26 cm3/s

In galaxy, 〈v〉 ∼ 10−3, ρDM ∼ 0.35 GeV/cm3

Excesses require 〈σv〉 ∼ 10−23 cm3/s

Perturbatively 〈σv〉 constant in v

Boost at low velocity up to αM/µ

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

The Need for Boost Factors

Annihilation Case

Early universe cross-section (v ∼ 0.2)

〈σv〉 ∼ 3× 10−26 cm3/s

In galaxy, 〈v〉 ∼ 10−3, ρDM ∼ 0.35 GeV/cm3

Excesses require 〈σv〉 ∼ 10−23 cm3/s

Perturbatively 〈σv〉 constant in v

Boost at low velocity up to αM/µ

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

Review of Sommerfeld Enhancement

s-Wave Enhancement for Annihilation

Annihilation local (` ∼ 1/M)Only s-wave allowed

Gauge force enhances wavefunctionvs plane-wave σ ∼ σ0|ψ(0)|2

Enhancement grows as α/vSaturates at ∼ αM/µ

Resonant enhancement if bound states

Higher Partial Wave

Relevant for scattering/exciting

Wavefunction in radius 1/µ

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

Review of Sommerfeld Enhancement

s-Wave Enhancement for Annihilation

Annihilation local (` ∼ 1/M)Only s-wave allowed

Gauge force enhances wavefunctionvs plane-wave σ ∼ σ0|ψ(0)|2

Enhancement grows as α/vSaturates at ∼ αM/µ

Resonant enhancement if bound states

Higher Partial Wave

Relevant for scattering/exciting

Wavefunction in radius 1/µ

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

A Difficulty for XDM

0 0.5 1 1.5u / a

0

0.1

0.2

0.3

0.4

0.5

Inte

gran

d

l = 0

l = 1

l = 2

Minimum Velocity

Excitation requires v ≥√

2δM/M

δM ∼ 2me, M ∼ TeV givesv & 10−3 about RMS velocity

Maxwell-Boltzmann suppression

〈σv〉 ∝∫ ∞

vmin

dvve−3v2/2v2rms

Need many partial wavesOnly few contribute

Difficult w/o very clumpy densityOr modified velocity profile

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

A Difficulty for XDM

Unitarity Limits

For partial wave l, σl ≤ π(2l + 1)/M2v2

Optimal mass (with MB distribution) near 700 GeV

Still requires density boost ×20Yukawa potential keeps large l contribution small

Standard XDM has trouble

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

A Difficulty for XDM

Unitarity Limits

For partial wave l, σl ≤ π(2l + 1)/M2v2

Optimal mass (with MB distribution) near 700 GeV

Still requires density boost ×20Yukawa potential keeps large l contribution small

Standard XDM has trouble

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

Inverting the DM Spectrum

Spectrum Inversion

Most models assume top spectrumSmall gap just spectator

But consider bottom spectrum

Middle state has small gap to jumpThen decay by e± pair

Inversion Benefits

Minimum velocity smaller than RMSReduces MB suppression

More partial waves contribute

Roughly optimized: M ∼ 500 GeV ,δM ∼ 86 keV , µ ∼ 120 MeV

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Sommerfeld

XDM Difficulty

New Spectrum

Model

Future

Inverting the DM Spectrum

Spectrum Inversion

Most models assume top spectrumSmall gap just spectator

But consider bottom spectrum

Middle state has small gap to jumpThen decay by e± pair

Inversion Benefits

Minimum velocity smaller than RMSReduces MB suppression

More partial waves contribute

Roughly optimized: M ∼ 500 GeV ,δM ∼ 86 keV , µ ∼ 120 MeV

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

An Inverted Model of Dark Matter

Goals

Engineer inverted DM spectrum for XDM

Keep middle population stable

Generate appropriate gauge boson mass & symmetrybreaking

Coupling to SM

XDM decay by e±

Annihilation spectrum (broad and peaked)

Find consistent cosmological history

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Particle Content and Interactions

SU(2) Gauge and DM Sector

Adjoint as SO(3) vector

Baµ = (Bµ, B

′µ, B

′′µ)

Majorana fermion DM χa

“Bare” mass ∼ 500 GeVInteractions as shown

Z2 symmetry

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Particle Content and Interactions

SU(2) Gauge and DM Sector

Adjoint as SO(3) vector

Baµ = (Bµ, B

′µ, B

′′µ)

Majorana fermion DM χa

“Bare” mass ∼ 500 GeVInteractions as shown

Z2 symmetry

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Particle Content and Interactions

Higgs Sector

Adjoint ∆a:

(∆a/Λ)BaµνY

µν

5-plet Σab:

hΣabχ̄aχb

Both add to Ba masses

Cosmological Sector

Heavy U(1) Z ′ (maybe)Coupled to eR

Heavy scalar S:

(S2/ΛGUT )χ̄aχa

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Particle Content and Interactions

Higgs Sector

Adjoint ∆a:

(∆a/Λ)BaµνY

µν

5-plet Σab:

hΣabχ̄aχb

Both add to Ba masses

Cosmological Sector

Heavy U(1) Z ′ (maybe)Coupled to eR

Heavy scalar S:

(S2/ΛGUT )χ̄aχa

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Symmetry Breaking

V = λ1

(ΣabΣab − 2Σ2

)2+λ2

(∆a∆a −∆2

)2+λ3∆aΣabΣbc∆c

+λ4∆aΣab∆b + λ5ΣabΣbcΣca

Scalar VEVs

〈∆1〉 = ∆, 〈∆0,2〉 = 0〈Σ01〉 = 〈Σ12〉 = 0 forλ3∆2 & λ5Σ〈Σ11〉 fixed, take small

〈Σ00〉 ∼ Σ, 〈Σ02〉 = 0

Gauge Boson Masses

µ = µ′′ = g√

2Σ2 + ∆2

〈Σ11〉 gives splitting

µ′ = g2√

2ΣTake ∆ >

√6Σ

So µ > µ′

∆ ∼ 10 GeV , Σ ∼ GeV ⇒ µ ∼ GeV , µ′ ∼ 100 MeV

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Symmetry Breaking

V = λ1

(ΣabΣab − 2Σ2

)2+λ2

(∆a∆a −∆2

)2+λ3∆aΣabΣbc∆c

+λ4∆aΣab∆b + λ5ΣabΣbcΣca

Scalar VEVs

〈∆1〉 = ∆, 〈∆0,2〉 = 0〈Σ01〉 = 〈Σ12〉 = 0 forλ3∆2 & λ5Σ〈Σ11〉 fixed, take small

〈Σ00〉 ∼ Σ, 〈Σ02〉 = 0

Gauge Boson Masses

µ = µ′′ = g√

2Σ2 + ∆2

〈Σ11〉 gives splitting

µ′ = g2√

2ΣTake ∆ >

√6Σ

So µ > µ′

∆ ∼ 10 GeV , Σ ∼ GeV ⇒ µ ∼ GeV , µ′ ∼ 100 MeV

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Symmetry Breaking

V = λ1

(ΣabΣab − 2Σ2

)2+λ2

(∆a∆a −∆2

)2+λ3∆aΣabΣbc∆c

+λ4∆aΣab∆b + λ5ΣabΣbcΣca

Scalar VEVs

〈∆1〉 = ∆, 〈∆0,2〉 = 0〈Σ01〉 = 〈Σ12〉 = 0 forλ3∆2 & λ5Σ〈Σ11〉 fixed, take small

〈Σ00〉 ∼ Σ, 〈Σ02〉 = 0

Gauge Boson Masses

µ = µ′′ = g√

2Σ2 + ∆2

〈Σ11〉 gives splitting

µ′ = g2√

2ΣTake ∆ >

√6Σ

So µ > µ′

∆ ∼ 10 GeV , Σ ∼ GeV ⇒ µ ∼ GeV , µ′ ∼ 100 MeV

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Symmetry Breaking

DM Mass Splittings

χ1 split from χ0, χ2 byloops

Yukawa splits χ0, χ2

δM ∼ 2hΣ ∼MeV

Plus splitting from 〈Σ11〉

Mass eigenbasis: M2

M1

M0

= M + αµ+

hΣ− 12α(µ− µ′)

0−hΣ− 1

2α(µ− µ′)

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Symmetry Breaking

DM Mass Splittings

χ1 split from χ0, χ2 byloops

Yukawa splits χ0, χ2

δM ∼ 2hΣ ∼MeV

Plus splitting from 〈Σ11〉

Mass eigenbasis: M2

M1

M0

= M + αµ+

hΣ− 12α(µ− µ′)

0−hΣ− 1

2α(µ− µ′)

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Excitation and Annihilation Signatures

Coupling to SM

B′ couples to hypercharge

Kinetic diagonalization

B′ = B̃′ + (∆/Λ) sin θW Z̃ + · · ·

No iDM for DAMA (due to Z2)

XDM and e± pairs

Enhanced χ1χ1 → χ2χ2 scattering

χ2 decays

Dominantly χ2 → e+e−χ0

Suppressed χ2 → γχ0

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Excitation and Annihilation Signatures

Coupling to SM

B′ couples to hypercharge

Kinetic diagonalization

B′ = B̃′ + (∆/Λ) sin θW Z̃ + · · ·

No iDM for DAMA (due to Z2)

XDM and e± pairs

Enhanced χ1χ1 → χ2χ2 scattering

χ2 decays

Dominantly χ2 → e+e−χ0

Suppressed χ2 → γχ0

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Excitation and Annihilation Signatures

Coupling to SM

B′ couples to hypercharge

Kinetic diagonalization

B′ = B̃′ + (∆/Λ) sin θW Z̃ + · · ·

No iDM for DAMA (due to Z2)

XDM and e± pairs

Enhanced χ1χ1 → χ2χ2 scattering

χ2 decays

Dominantly χ2 → e+e−χ0

Suppressed χ2 → γχ0

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Excitation and Annihilation Signatures

Annihilation

χ0χ0 or χ1χ1 as before

B′ produced dominantly on-shellHence only e±

Two e± pairs, so broad spectrum

Z ′ (introduced later) → e± pair

Much sharper spectrum

ATIC peak?

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Cosmology of DM Sector

DM Thermal Relic Density

Freeze-out density ∼ 1/σχ abundance too high

Either increase gauge couplingOr introduce new Z ′

Z ′ would add to ATIC peak

Gauge & Scalar Relics

Similar but lower mass propagators

Negligible abundances

Signals entirely too weak

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Cosmology of DM Sector

DM Thermal Relic Density

Freeze-out density ∼ 1/σχ abundance too high

Either increase gauge couplingOr introduce new Z ′

Z ′ would add to ATIC peak

Gauge & Scalar Relics

Similar but lower mass propagators

Negligible abundances

Signals entirely too weak

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Cosmology of DM Sector

Kinetic Equilibration

Consider χχ↔ χχ scatteringEquilibrium at low KE depletes χ1

At KE∼ 2me, v ∼ 10−3

Sommerfeld enhanced

Note p ∝ a−1 ∝ TSo 〈σv〉 ∝ 1/v ∝ 1/T , n〈σv〉 ∝ H

More p removes equilibration

Nonthermal Generation

Take mS ∼ 〈S〉 ∼ ΛThermal WIMP abundance

Induced Yukawa with χ

Decay rate:

mS(〈S〉/ΛGUT )2

Need low χ freeze-out

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Particle Content

Higgsing

Signatures

Cosmology

Future

Cosmology of DM Sector

Kinetic Equilibration

Consider χχ↔ χχ scatteringEquilibrium at low KE depletes χ1

At KE∼ 2me, v ∼ 10−3

Sommerfeld enhanced

Note p ∝ a−1 ∝ TSo 〈σv〉 ∝ 1/v ∝ 1/T , n〈σv〉 ∝ H

More p removes equilibration

Nonthermal Generation

Take mS ∼ 〈S〉 ∼ ΛThermal WIMP abundance

Induced Yukawa with χ

Decay rate:

mS(〈S〉/ΛGUT )2

Need low χ freeze-out

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

Future Directions

Quantum Mechanics

Improved studies of multistate Sommerfeld enhancementWKB when numerics are too difficult

Particle Physics

More detailed exploration of the model

Can other reps work for iDM?

Cosmology

Advantages of nonthermal generation?

More detailed calculation of signals

Dark matter is exciting right now!

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

Future Directions

Quantum Mechanics

Improved studies of multistate Sommerfeld enhancementWKB when numerics are too difficult

Particle Physics

More detailed exploration of the model

Can other reps work for iDM?

Cosmology

Advantages of nonthermal generation?

More detailed calculation of signals

Dark matter is exciting right now!

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

Future Directions

Quantum Mechanics

Improved studies of multistate Sommerfeld enhancementWKB when numerics are too difficult

Particle Physics

More detailed exploration of the model

Can other reps work for iDM?

Cosmology

Advantages of nonthermal generation?

More detailed calculation of signals

Dark matter is exciting right now!

Inverted XDM

ARF

Outline

DM Hints

Boost Factors

Model

Future

Future Directions

Quantum Mechanics

Improved studies of multistate Sommerfeld enhancementWKB when numerics are too difficult

Particle Physics

More detailed exploration of the model

Can other reps work for iDM?

Cosmology

Advantages of nonthermal generation?

More detailed calculation of signals

Dark matter is exciting right now!