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!