Thermal Sneutrino Dark Matter Thermal Sneutrino Dark Matter in the in the FFDD-Term Model of Hybrid Inflation-Term Model of Hybrid Inflation
The
Uni
vers
ity
of M
anch
este
r
Frank [email protected]
University of Manchester
in collaboration with A. Pilaftsis
FFD, A. Pilaftsis, JHEP 0810 (2008) 080
Particle Physics Seminar Oxford, 7 May 2009
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model22/40/40
OverviewOverview
IntroductionDark Matter EvidenceSupersymmetryNeutrino Physics
FD Term Hybrid ModelSuperpotentialInflaton VEVHybrid Inflation
RH Sneutrino Dark MatterMass Spectrum
Annihilation
Conclusion
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Evidence for Dark MatterEvidence for Dark Matter
Cluster FormationGalactic Rotation CurvesGravitational LensingCMB FluctuationsLarge Scale StructureStandard Cosmological Model:
Cold Dark Matter Component of the Universe
CDM h2≈0.11
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SupersymmetrySupersymmetryMSSM: Minimal extension of the Standard Model with two Higgs doublets and conserved R-parity
http://www.physics.gla.ac.uk/ppt/susy.htm
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model55/40/40
SupersymmetrySupersymmetryMSSM: Minimal extension of the Standard Model with two Higgs doublets and conserved R-parity
SUSY must be broken⇒ In general: Introduction of more than 100 free parameters⇒ Required: Theoretical framework for SUSY breaking⇒ Minimal Supergravity (mSUGRA), Universality at GUT Scale
http://www.physics.gla.ac.uk/ppt/susy.htm
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Neutrino Oscillations⇒ Mixing angles and mass differences
Absolute Mass Scale
NeutrinosNeutrinos
sin212=0.30−0.050.04 ,sin223=0.50−0.12
0.14 ,sin2130.028m12
2 =8.1−0.60.6⋅10−5 eV2 ,m13
2 =±2.2−0.50.7⋅10−3 eV2
m10.5eV
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Neutrino Oscillations⇒ Mixing angles and mass differences
Absolute Mass Scale
Seesaw Mechanism⇒ Add heavy right-handed neutrinos
But: With suitable flavor symmetry in MR and mD, right-handed neutrinos can be as light as 100 GeV
NeutrinosNeutrinos
sin212=0.30−0.050.04 ,sin223=0.50−0.12
0.14 ,sin2130.028m12
2 =8.1−0.60.6⋅10−5 eV2 ,m13
2 =±2.2−0.50.7⋅10−3 eV2
m10.5eV
0 mDT
mD M R ⇒ m≈0.1eV mD
100GeV 2
M R
1014GeV −1
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FFDD-Term Hybrid Model-Term Hybrid Model
Extension of the MSSMW=W MSSM=0
Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06
A Minimal Particle-Cosmology Supersymmetric Model
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model99/40/40
FFDD-Term Hybrid Model-Term Hybrid Model
Extension of the MSSMInflaton-Waterfall sector
W=W MSSM=0
S X 1X 2−M 2
Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06
A Minimal Particle-Cosmology Supersymmetric Model
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1010/40/40
FFDD-Term Hybrid Model-Term Hybrid Model
Extension of the MSSMInflaton-Waterfall sector
Effective µ term, µ = λ ⟨S⟩
W=W MSSM=0
S X 1X 2−M 2
S H uH d
Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06
A Minimal Particle-Cosmology Supersymmetric Model
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1111/40/40
FFDD-Term Hybrid Model-Term Hybrid Model
Extension of the MSSMInflaton-Waterfall sector
Effective µ term, µ = λ ⟨S⟩Effective neutrino Majorana mass, M = ρ ⟨S⟩Neutrino Yukawa coupling
W=W MSSM=0
S X 1X 2−M 2
S H uH d
ij
2S N i
N j
hij Li
H uN j
Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06
A Minimal Particle-Cosmology Supersymmetric Model
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1212/40/40
FFDD-Term Hybrid Model-Term Hybrid Model
Extension of the MSSMInflaton-Waterfall sector
Effective µ term, µ = λ ⟨S⟩Effective neutrino Majorana mass, M = ρ ⟨S⟩Neutrino Yukawa coupling
Fayet-Iliopoulos D-Term
W=W MSSM=0
S X 1X 2−M 2
S H uH d
ij
2S N i
N j
hij Li
H uN j
−g X
2mFI
2 D X
Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06
A Minimal Particle-Cosmology Supersymmetric Model
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1313/40/40
Inflaton VEVInflaton VEV
Soft SUSY breaking Lagrangian
−Lsoft⊃M S2 S∗ SM N
2 N i∗ N i A S X 1 X 2 AS H u H d
ij
2A S N i
N j−a S M 2 S
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1414/40/40
Inflaton VEVInflaton VEV
Soft SUSY breaking Lagrangian
Scalar Potential ( ⟨X1,2⟩ = M )
−Lsoft⊃M S2 S∗ SM N
2 N i∗ N i A S X 1 X 2 AS H u H d
ij
2A S N i
N j−a S M 2 S
V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣
2M S2 S∗ S[M 2A−aS Sh.c.]
=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1515/40/40
Inflaton VEVInflaton VEV
Soft SUSY breaking Lagrangian
Scalar Potential ( ⟨X1,2⟩ = M )
Inflaton VEV (κ ≈ λ ≈ ρ ≈ 10−2)
−Lsoft⊃M S2 S∗ SM N
2 N i∗ N i A S X 1 X 2 AS H u H d
ij
2A S N i
N j−a S M 2 S
V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣
2M S2 S∗ S[M 2A−aS Sh.c.]
=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]
⟨S ⟩= 12∣A−aS∣O M SUSY
2 /M ≈102 M SUSY
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Inflaton VEVInflaton VEV
Soft SUSY breaking Lagrangian
Scalar Potential ( ⟨X1,2⟩ = M )
Inflaton VEV (κ ≈ λ ≈ ρ ≈ 10−2)
−Lsoft⊃M S2 S∗ SM N
2 N i∗ N i A S X 1 X 2 AS H u H d
ij
2A S N i
N j−a S M 2 S
V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣
2M S2 S∗ S[M 2A−aS Sh.c.]
=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]
⟨S ⟩= 12∣A−aS∣O M SUSY
2 /M ≈102 M SUSY
=⟨S ⟩≈M SUSY
µ-Parametermij
N=ij ⟨S ⟩≈M SUSY
Majorana Mass Matrix
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FFDD-Term Hybrid Inflation-Term Hybrid Inflation
Hybrid Inflation (Linde '91)
New scalar field ends inflation by acquiring VEV
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1818/40/40
FFDD-Term Hybrid Inflation-Term Hybrid Inflation
Hybrid Inflation (Linde '91)
New scalar field ends inflation by acquiring VEV
F-Term Hybrid Inflation(Copeland et al., Dvali, Shafi, Schaefer '94)
Waterfall Fields X1, X2
Scalar Potential from F terms and supergravity/loop corrections
W= S X 1X 2−M 2
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model1919/40/40
FFDD-Term Hybrid Inflation-Term Hybrid Inflation
Hybrid Inflation (Linde '91)
New scalar field ends inflation by acquiring VEV
F-Term Hybrid Inflation(Copeland et al., Dvali, Shafi, Schaefer '94)
Waterfall Fields X1, X2
Scalar Potential from F terms and supergravity/loop corrections
FD-Term Hybrid Inflation (Garbrecht, Pilaftsis '06)
Subdominant non-anomalous FI D-term breaking discrete D-parity in waterfall sectorU(1)X gauge sector fields can decay ⇒ entropy release ⇒ avoid gravitino overabundance problem
W= S X 1X 2−M 2
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Constraints from InflationConstraints from Inflation
Bounds on model parameters κ, λ, ρ fromNumber of e-folds
Power spectrum of curvature perturbations
Spectral index
N e=1
mPl2 ∫end
exit
d V inf
V inf' ≈55
P R1/2= 1
23mPl
V inf3/2exit
V inf' exit
≈4.86⋅10−5
ns−1=2mPl2 V inf
' ' exitV inf exit
=−0.037−0.0150.014
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model2121/40/40
Constraints from InflationConstraints from Inflation
Spectral Index
Slow-roll slope from SUGRA and radiative corrections
≈≈23.2⋅10−2⇒ At inflationary scale M≈1016 GeV for minimal (next-to-minimal) Kähler potential
≈≈1.11.8⋅10−2⇒ At EW scale
RG Evolution
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model2222/40/40
Sneutrino Mass SpectrumSneutrino Mass Spectrum
FD-Term Model conserves R-parity → LSP is stable
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Sneutrino Mass SpectrumSneutrino Mass Spectrum
FD-Term Model conserves R-parity → LSP is stableRight-Handed Sneutrino Mass Matrix(small Yukawa interactions with LH sneutrinos neglected)
→ 3 Heavy and 3 Light Right-Handed Sneutrinos
→ Lightest Right-Handed Sneutrino can be LSP
N 1,2,3 , N 1,2,3∗ T 2 vS
2M N2 Avu vd
A∗vu vd 2 vS
2M N2 N 1,2,3
N 1,2,3∗
m N LSP
2 =2 vS2M N
2 −∣ AvSvu vd∣
≈2m02−∣A0∣, mSUGRA, tan ≫1,=≪1
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Right-Handed Sneutrino LSP Right-Handed Sneutrino LSP Scan over mSUGRA parameters (A0 = 300 GeV, µ > 0, tanβ = 10,30)
Sneutrino LSP points to low-energy SUSY spectrum, consistent with annihilation via Higgs m N 1
≈20−100 GeV
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model2525/40/40
Sneutrino Cold Dark MatterSneutrino Cold Dark Matter
MSSM (+ RH Neutrinos)Left-Handed Sneutrino LSP
Annihilates too efficiently (gauge interaction)
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Sneutrino Cold Dark MatterSneutrino Cold Dark Matter
MSSM (+ RH Neutrinos)Left-Handed Sneutrino LSP
Annihilates too efficiently (gauge interaction)
Right-Handed Sneutrino LSPOvercloses Universe as thermal DM (small Yukawa interaction)
Possible as non-thermal DM (Gopalakrishna, de Gouvêa, Porod '06)
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model2727/40/40
Sneutrino Cold Dark MatterSneutrino Cold Dark Matter
MSSM (+ RH Neutrinos)Left-Handed Sneutrino LSP
Annihilates too efficiently (gauge interaction)
Right-Handed Sneutrino LSPOvercloses Universe as thermal DM (small Yukawa interaction)
Possible as non-thermal DM (Gopalakrishna, de Gouvêa, Porod '06)
Left-Right Mixtures possible (Arina, Fornengo '06)
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Sneutrino Cold Dark MatterSneutrino Cold Dark Matter
MSSM (+ RH Neutrinos)Left-Handed Sneutrino LSP
Annihilates too efficiently (gauge interaction)
Right-Handed Sneutrino LSPOvercloses Universe as thermal DM (small Yukawa interaction)
Possible as non-thermal DM (Gopalakrishna, de Gouvêa, Porod '06)
Left-Right Mixtures possible (Arina, Fornengo '06)
FD-Term Model → New Interaction12 N i
∗ N i∗H u H dh.c. F S=
12 N i
N i H uH dfrom inflaton F-term
Quartic Coupling to Higgs Fields (McDonald '94, Burgess et al. '01)
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Annihilation ChannelsAnnihilation Channels
12
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Dark Matter SearchesDark Matter Searches
Direct SearchesElastic Scattering between Sneutrino and Nucleus
via t-channel Higgs exchangePer Nucleon
Experiments: CDMS-II, SuperCDMS, Xenon1T
elnucleon≈5⋅10−50 cm2 10−4
2
100GeVmH 1
4
50GeVm N 1
2
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model3131/40/40
Dark Matter SearchesDark Matter Searches
Direct SearchesElastic Scattering between Sneutrino and Nucleus
via t-channel Higgs exchangePer Nucleon
Experiments: CDMS-II, SuperCDMS, Xenon1T
Indirect SearchesDetection of Dark Matter annihilation products
such as photons, positrons, anti-protonsHigh-energy Neutrinos from Sun and Earth
elnucleon≈5⋅10−50 cm2 10−4
2
100GeVmH 1
4
50GeVm N 1
2
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Sneutrino AnnihilationSneutrino Annihilation
Calculation of Sneutrino Relic Density
Higgs properties calculated using CPSuperH (Lee at al. '03)
Annihilation via Higgs
Inflationary Bounds
Direct WIMP Searches
DM h2=0.11
Scenario I: m0=70 GeV, m1/2=243 GeV, A0=300 GeV, tanβ =10, µ =303 GeV
m N 1≈mH 1
/22⋅10−4
2.35.8⋅10−4
≈10−1...−3
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Sneutrino AnnihilationSneutrino Annihilation
Scenario II: m0=125 GeV, m1/2=212 GeV, A0=300 GeV, tanβ =30, µ =263 GeV
DM h2=0.11
Calculation of Sneutrino Relic Density
Higgs properties calculated using CPSuperH (Lee at al. '03)
Annihilation via Higgs
Inflationary Bounds
Direct WIMP Searches
m N 1≈mH 1
/22⋅10−4
2.35.8⋅10−4
≈10−1...−3
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Sneutrino AnnihilationSneutrino Annihilation
Scenario II: m0=125 GeV, m1/2=212 GeV, A0=300 GeV, tanβ =30, µ =263 GeV
DM h2=0.11
Calculation of Sneutrino Relic Density
Higgs properties calculated using CPSuperH (Lee at al. '03)
Annihilation via Higgs
Inflationary Bounds
Direct WIMP Searches
m N 1≈mH 1
/22⋅10−4
2.35.8⋅10−4
≈10−1...−3
H ere be H umans
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ConclusionConclusion
FD-Term Model providesInflationary Mechanism
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ConclusionConclusion
FD-Term Model providesInflationary MechanismSolution to Gravitino Problem
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ConclusionConclusion
FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ Problem
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ConclusionConclusion
FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy Neutrinos
Seesaw MechanismResonant LeptogenesisLepton Flavor Violating ProcessesAccessible at LHC?
7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model3939/40/40
ConclusionConclusion
FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy NeutrinosRight-Handed Sneutrinos as Thermal DM
Low Energy SUSY SpectrumAnnihilation via Higgs Funnel m N LSP
=mH 1/2≈60GeV
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ConclusionConclusion
FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy NeutrinosRight-Handed Sneutrinos as Thermal DM
Low Energy SUSY SpectrumAnnihilation via Higgs FunnelInvisible Higgs DecaysSneutrinos within Cascade Decays
m N LSP=mH 1
/2≈60GeV