Composite Dark Matter and insights from the Lattice Enrico Rinaldi - - PowerPoint PPT Presentation
Lattice 2016 Southampton, UK Composite Dark Matter and insights from the Lattice Enrico Rinaldi This research was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract
This research was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and supported by the LLNL LDRD “Illuminating the Dark Universe with PetaFlops Supercomputing” 13-ERD-023. Computing support comes from the LLNL Institutional Computing Grand Challenge program. LLNL-PRES-669543
Lattice 2016 Southampton, UK
and insights from the Lattice
Enrico Rinaldi
[Hubble + Plank/ESA]
[Hubble + Plank/ESA]
[Hubble + Plank/ESA]
[Hubble + Plank/ESA]
𝜍DM ≈ 5 ρSM
Direct Detection Indirect Detection Production at Colliders
DM DM SM SM
Direct Detection Indirect Detection Production at Colliders
DM DM SM SM
Direct Detection Indirect Detection Production at Colliders
DM DM SM SM
Direct Detection Indirect Detection Production at Colliders
DM DM SM SM
What is Dark Matter?
What is Dark Matter?
mSUGRA R-parity Conserving
Supersymmetry
pMSSM R-parity violating Gravitino DM
MSSM
NMSSM
Dirac DMExtra Dimensions
UED DM
Warped Extra Dimensions
Little Higgs
T
Axion-like Particles QCD Axions
Axion DM
Sterile Neutrinos
Light Force Carriers
Dark Photon
Asymmetric DM
RS DM
Warm DM
Hidden Sector DM WIMPless DM
Littlest Higgs
Self-Interacting DM Q-balls
T Tait
Solitonic DM
Quark Nuggets Techni- baryons
Dynamical DM[Planning the Future of U.S. Particle Physics (Snowmass 2013), 1401.6085]
What is Dark Matter?
mSUGRA R-parity Conserving
Supersymmetry
pMSSM R-parity violating Gravitino DM
MSSM
NMSSM
Dirac DMExtra Dimensions
UED DM
Warped Extra Dimensions
Little Higgs
T
Axion-like Particles QCD Axions
Axion DM
Sterile Neutrinos
Light Force Carriers
Dark Photon
Asymmetric DM
RS DM
Warm DM
Hidden Sector DM WIMPless DM
Littlest Higgs
Self-Interacting DM Q-balls
T Tait
Solitonic DM
Quark Nuggets Techni- baryons
Dynamical DM[Planning the Future of U.S. Particle Physics (Snowmass 2013), 1401.6085]
★ Gravitational effects of DM show up in CMB, lensing and other large scale phenomena ★ Direct Standard Model interactions are needed for production in the early Universe ★ Direct detection and Collider experiments rely on SM interactions, but they are suppressed ★ Strong exclusion bounds push theorists to explore a wider landscape of models for DM ★ Problems with cosmological models can hint at strongly self-interacting dark matter
mSUGRA R-parity Conserving
Supersymmetry
pMSSM R-parity violating Gravitino DM
MSSM
NMSSM
Dirac DMExtra Dimensions
UED DM
Warped Extra Dimensions
Little Higgs
T
Axion-like Particles QCD Axions
Axion DM
Sterile Neutrinos
Light Force Carriers
Dark Photon
Asymmetric DM
RS DM
Warm DM
Hidden Sector DM WIMPless DM
Littlest Higgs
Self-Interacting DM Q-balls
T Tait
Solitonic DM
Quark Nuggets Techni- baryons
Dynamical DM[Planning the Future of U.S. Particle Physics (Snowmass 2013), 1401.6085]
Composite Dark Matter
Composite Dark Matter
✦ Dark Matter is a composite object
Composite Dark Matter
✦ Dark Matter is a composite object
e.g. technibaryon or hidden glueball
Composite Dark Matter
✦ Dark Matter is a composite object ✦ Interesting and complicated internal
structure
✦ Properties dictated by strong dynamics ✦ Self-interactions are natural
e.g. technibaryon or hidden glueball
Composite Dark Matter
✦ Dark Matter is a composite object ✦ Interesting and complicated internal
structure
✦ Properties dictated by strong dynamics ✦ Self-interactions are natural
e.g. technibaryon or hidden glueball
Similar to QCD
Composite Dark Matter
✦ Dark Matter is a composite object ✦ Interesting and complicated internal
structure
✦ Properties dictated by strong dynamics ✦ Self-interactions are natural ✦ Composite object is neutral ✦ Constituents may interact with Standard
Model particles
e.g. technibaryon or hidden glueball
Similar to QCD
Composite Dark Matter
✦ Dark Matter is a composite object ✦ Interesting and complicated internal
structure
✦ Properties dictated by strong dynamics ✦ Self-interactions are natural ✦ Composite object is neutral ✦ Constituents may interact with Standard
Model particles
e.g. technibaryon or hidden glueball
Similar to QCD Chance to observe them in experiments and give the correct relic abundance
Composite Dark Matter
✦ Dark Matter is a composite object ✦ Interesting and complicated internal
structure
✦ Properties dictated by strong dynamics ✦ Self-interactions are natural ✦ Composite object is neutral ✦ Constituents may interact with Standard
Model particles
e.g. technibaryon or hidden glueball
Similar to QCD Chance to observe them in experiments and give the correct relic abundance
Lattice Field Theory methods
Natural features of Composite Dark Matter
[review by Kribs & Neil, 1604.04627]
Natural features of Composite Dark Matter
[review by Kribs & Neil, 1604.04627]
Stability is a direct consequence of accidental symmetries
Natural features of Composite Dark Matter
[review by Kribs & Neil, 1604.04627]
Stability is a direct consequence of accidental symmetries Neutrality follows naturally from confinement into singlet
Natural features of Composite Dark Matter
[review by Kribs & Neil, 1604.04627]
Stability is a direct consequence of accidental symmetries Neutrality follows naturally from confinement into singlet
Small interactions with SM particles arise from form factor suppression (higher
Natural features of Composite Dark Matter
[review by Kribs & Neil, 1604.04627]
Stability is a direct consequence of accidental symmetries Neutrality follows naturally from confinement into singlet
Small interactions with SM particles arise from form factor suppression (higher
Self-interactions are included due to strongly coupled dynamics
Models for Composite Dark Matter
★ Pion-like (dark quark-antiquark) ✦ pNGB DM [Hietanen et al.,1308.4130] ✦ Quirky DM [Kribs et al.,0909.2034] ✦ Ectocolor DM [Buckley&Neil,1209.6054] ✦ SIMP [Hochberg et al.,1411.3727] ✦ Minimal SU(2) [Lewis, Wed.@11:50]
[review by Kribs & Neil, 1604.04627] [list of references focused on lattice results when possible]
★ Baryon-like (multiple quarks) ✦ “Technibaryons” [LSD,1301.1693] ✦ Stealth DM [LSD,1503.04203-1503.04205] ✦ One-family TC [LatKMI,1510.07373] ✦ Sextet CH [LatHC,1601.03302][Kuti, Mon.@15:15]
Models for Composite Dark Matter
★ Pion-like (dark quark-antiquark) ✦ pNGB DM [Hietanen et al.,1308.4130] ✦ Quirky DM [Kribs et al.,0909.2034] ✦ Ectocolor DM [Buckley&Neil,1209.6054] ✦ SIMP [Hochberg et al.,1411.3727] ✦ Minimal SU(2) [Lewis, Wed.@11:50]
[review by Kribs & Neil, 1604.04627] [list of references focused on lattice results when possible]
★ Baryon-like (multiple quarks) ✦ “Technibaryons” [LSD,1301.1693] ✦ Stealth DM [LSD,1503.04203-1503.04205] ✦ One-family TC [LatKMI,1510.07373] ✦ Sextet CH [LatHC,1601.03302][Kuti, Mon.@15:15]
Models for Composite Dark Matter
★ Pion-like (dark quark-antiquark) ✦ pNGB DM [Hietanen et al.,1308.4130] ✦ Quirky DM [Kribs et al.,0909.2034] ✦ Ectocolor DM [Buckley&Neil,1209.6054] ✦ SIMP [Hochberg et al.,1411.3727] ✦ Minimal SU(2) [Lewis, Wed.@11:50]
[review by Kribs & Neil, 1604.04627]
★Glueball-like (only gluons) ✦ SUNonia [Boddy et al.,1402.3629]
[Soni, Wed.@11:30]
[list of references focused on lattice results when possible]
★ Baryon-like (multiple quarks) ✦ “Technibaryons” [LSD,1301.1693] ✦ Stealth DM [LSD,1503.04203-1503.04205] ✦ One-family TC [LatKMI,1510.07373] ✦ Sextet CH [LatHC,1601.03302][Kuti, Mon.@15:15]
Models for Composite Dark Matter
★ Pion-like (dark quark-antiquark) ✦ pNGB DM [Hietanen et al.,1308.4130] ✦ Quirky DM [Kribs et al.,0909.2034] ✦ Ectocolor DM [Buckley&Neil,1209.6054] ✦ SIMP [Hochberg et al.,1411.3727] ✦ Minimal SU(2) [Lewis, Wed.@11:50]
[review by Kribs & Neil, 1604.04627]
★Glueball-like (only gluons) ✦ SUNonia [Boddy et al.,1402.3629]
[Soni, Wed.@11:30]
★Dark Nuclei [Detmold et
al.,1406.2276-1406.4116]
[list of references focused on lattice results when possible]
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290]
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290] [Chivukula et al.,hep-ph/9210274]
Relevant if the constituents have SM color charges
[Godbole et al.,1506.01408] [Bay&Osborne,1506.07110]
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290] [Chivukula et al.,hep-ph/9210274]
Relevant if the constituents have SM color charges
[Godbole et al.,1506.01408] [Bay&Osborne,1506.07110]
Lowest dimensional operators:
★ magnetic dipole (5) ★ charge radius (6) ★ polarizability (7)
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290]
Same as γ but suppressed due to heavy mass
[Chivukula et al.,hep-ph/9210274]
Relevant if the constituents have SM color charges
[Godbole et al.,1506.01408] [Bay&Osborne,1506.07110]
Lowest dimensional operators:
★ magnetic dipole (5) ★ charge radius (6) ★ polarizability (7)
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290]
Same as γ but suppressed due to heavy mass Most relevant interaction if constituents have Yukawa couplings!
[Chivukula et al.,hep-ph/9210274]
Relevant if the constituents have SM color charges
[Godbole et al.,1506.01408] [Bay&Osborne,1506.07110]
Lowest dimensional operators:
★ magnetic dipole (5) ★ charge radius (6) ★ polarizability (7)
The darkness of Composite Dark Matter
[Wikipedia] [Bagnasco et al., hep-ph/9310290]
Same as γ but suppressed due to heavy mass Most relevant interaction if constituents have Yukawa couplings!
[Chivukula et al.,hep-ph/9210274]
Relevant if the constituents have SM color charges
[Godbole et al.,1506.01408] [Bay&Osborne,1506.07110]
Lowest dimensional operators:
★ magnetic dipole (5) ★ charge radius (6) ★ polarizability (7)
Lattice results for Composite Dark Matter
SU(2) Nf=1 SU(2) Nf=2 SU(3) Nf=2,6 SU(3) Nf=2 (S) SU(4) Nf=4 SO(4) Nf=2 (V) SU(N) Nf=0
Template Models
Spectrum Higgs
Charge r. Polariz. SU(3) Nf=8
lattice estimate [references in Kribs & Neil, 1604.04627] [Talk by Lewis, Wed.@11.50, new simulations are in progress] [Talk by Kuti, Mon.@15.15, small component of DM and tree-level interaction with Z boson] [Talk by Soni, Wed.@11.30, interested in calculating self-interactions on the lattice] forbidden
Lattice results for Composite Dark Matter
SU(2) Nf=1 SU(2) Nf=2 SU(3) Nf=2,6 SU(3) Nf=2 (S) SU(4) Nf=4 SO(4) Nf=2 (V) SU(N) Nf=0
Template Models
Spectrum Higgs
Charge r. Polariz. SU(3) Nf=8
lattice estimate [references in Kribs & Neil, 1604.04627] [Talk by Lewis, Wed.@11.50, new simulations are in progress] [Talk by Kuti, Mon.@15.15, small component of DM and tree-level interaction with Z boson] forbidden in Stealth DM forbidden in pNGB DM forbidden in SUNonia forbidden
Computing Higgs exchange
✦ Need to non-perturbatively evaluate the dark σ-term
Ma = yfyq 2m2
h
X
f
hB| ¯ ff|Bi X
q
ha|¯ qq|ai
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373]
h
[DeGrand et al., 1501.05665]
Computing Higgs exchange
✦ Need to non-perturbatively evaluate the dark σ-term
Ma = yfyq 2m2
h
X
f
hB| ¯ ff|Bi X
q
ha|¯ qq|ai
1. effective Higgs coupling with dark fermions and quark Yukawa coupling 2. dark baryon scalar form factor: need lattice input for generic DM models! 3. nucleon scalar form factor: ChPT and lattice input
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373] [Plenary talk by Collins, Tue@10:15]
h
[DeGrand et al., 1501.05665]
Computing Higgs exchange
✦ Need to non-perturbatively evaluate the dark σ-term ✦ Effective Higgs coupling non- trivial with mixed chiral and vector-like masses
Ma = yfyq 2m2
h
X
f
hB| ¯ ff|Bi X
q
ha|¯ qq|ai
1. effective Higgs coupling with dark fermions and quark Yukawa coupling 2. dark baryon scalar form factor: need lattice input for generic DM models! 3. nucleon scalar form factor: ChPT and lattice input yfhB| ¯ ff|Bi = mB v X
f
v mf ∂ mf(h) ∂ h
f (B)
f
mf(h) = m + yfh √ 2
α ≡ v mf ∂ mf(h) ∂ h
= yv √ 2m + yv
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373] [Plenary talk by Collins, Tue@10:15]
h
[DeGrand et al., 1501.05665]
Computing Higgs exchange
✦ Need to non-perturbatively evaluate the dark σ-term ✦ Effective Higgs coupling non- trivial with mixed chiral and vector-like masses ✦ Model-dependent answer for the cross-section
Ma = yfyq 2m2
h
X
f
hB| ¯ ff|Bi X
q
ha|¯ qq|ai
1. effective Higgs coupling with dark fermions and quark Yukawa coupling 2. dark baryon scalar form factor: need lattice input for generic DM models! 3. nucleon scalar form factor: ChPT and lattice input yfhB| ¯ ff|Bi = mB v X
f
v mf ∂ mf(h) ∂ h
f (B)
f
mf(h) = m + yfh √ 2
α ≡ v mf ∂ mf(h) ∂ h
= yv √ 2m + yv
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373] [Plenary talk by Collins, Tue@10:15]
h
[DeGrand et al., 1501.05665]
Computing Higgs exchange
✦ Need to non-perturbatively evaluate the dark σ-term ✦ Effective Higgs coupling non- trivial with mixed chiral and vector-like masses ✦ Model-dependent answer for the cross-section ✦ Lattice input is necessary: compute mass and form factor
Ma = yfyq 2m2
h
X
f
hB| ¯ ff|Bi X
q
ha|¯ qq|ai
1. effective Higgs coupling with dark fermions and quark Yukawa coupling 2. dark baryon scalar form factor: need lattice input for generic DM models! 3. nucleon scalar form factor: ChPT and lattice input yfhB| ¯ ff|Bi = mB v X
f
v mf ∂ mf(h) ∂ h
f (B)
f
mf(h) = m + yfh √ 2
α ≡ v mf ∂ mf(h) ∂ h
= yv √ 2m + yv
Lattice!
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373] [Plenary talk by Collins, Tue@10:15]
h
[DeGrand et al., 1501.05665]
Bounds from Higgs exchange
1000 10000 mB [GeV] 1e-42 1e-40 1e-38 1e-36 σ0 [cm
2]
SU(3) Nf=8 “technibaryon” SU(4) Nf=4 Stealth DM
MPSêMV=0.77
10 50 100 500 1000 1¥10-46 5¥10-46 1¥10-45 5¥10-45 1¥10-44 5¥10-44 1¥10-43 5¥10-43 mBHGeVL DM-nucleon cross section Hcm2L
훼 = . 6 4 훼 = . 1 6 훼 = . 4 훼 = . 1
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373]
✦Lattice results for the cross-section are compared to experimental bounds ✦Coupling space in specific models can be vastly constrained
[DeGrand et al., 1501.05665]
✦Some candidates can be excluded as dominant sources
✦There is lattice evidence for universality of dark scalar form factors
h
Bounds from Higgs exchange
1000 10000 mB [GeV] 1e-42 1e-40 1e-38 1e-36 σ0 [cm
2]
SU(3) Nf=8 “technibaryon” SU(4) Nf=4 Stealth DM
MPSêMV=0.77
10 50 100 500 1000 1¥10-46 5¥10-46 1¥10-45 5¥10-45 1¥10-44 5¥10-44 1¥10-43 5¥10-43 mBHGeVL DM-nucleon cross section Hcm2L
훼 = . 6 4 훼 = . 1 6 훼 = . 4 훼 = . 1
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373]
Purely Yukawa mass is excluded
✦Lattice results for the cross-section are compared to experimental bounds ✦Coupling space in specific models can be vastly constrained
[DeGrand et al., 1501.05665]
✦Some candidates can be excluded as dominant sources
✦There is lattice evidence for universality of dark scalar form factors
h
Bounds from Higgs exchange
1000 10000 mB [GeV] 1e-42 1e-40 1e-38 1e-36 σ0 [cm
2]
SU(3) Nf=8 “technibaryon” SU(4) Nf=4 Stealth DM
MPSêMV=0.77
10 50 100 500 1000 1¥10-46 5¥10-46 1¥10-45 5¥10-45 1¥10-44 5¥10-44 1¥10-43 5¥10-43 mBHGeVL DM-nucleon cross section Hcm2L
훼 = . 6 4 훼 = . 1 6 훼 = . 4 훼 = . 1
[LSD, 1402.6656-1503.04203] [LatKMI, 1510.07373]
Purely Yukawa mass is excluded
✦Lattice results for the cross-section are compared to experimental bounds ✦Coupling space in specific models can be vastly constrained
[DeGrand et al., 1501.05665]
✦Some candidates can be excluded as dominant sources
✦There is lattice evidence for universality of dark scalar form factors
h
Bounds from EM moments
10−2 10−1 100 101 102 Mχ = MB [TeV] 10−16 10−14 10−12 10−10 10−8 10−6 10−4 10−2 100 102 104 Rate, event / (kg·day)
Nf = 2 Nf = 6 XENON100 [1207.5988], 95% CL exclusion
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
★ baryon similar to QCD neutron ★ dark quarks with Q=Y ★ calculate connected 3pt ★ scale set by DM mass ★ magnetic moment dominates ★ results independent of Nf
[LSD, 1301.1693]
SU(3) Nf=2,6 dark fermionic baryon
Bounds from EM moments
10−2 10−1 100 101 102 Mχ = MB [TeV] 10−16 10−14 10−12 10−10 10−8 10−6 10−4 10−2 100 102 104 Rate, event / (kg·day)
Nf = 2 Nf = 6 XENON100 [1207.5988], 95% CL exclusion
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
★ baryon similar to QCD neutron ★ dark quarks with Q=Y ★ calculate connected 3pt ★ scale set by DM mass ★ magnetic moment dominates ★ results independent of Nf
[LSD, 1301.1693]
SU(3) Nf=2,6 dark fermionic baryon
Excluded MB >~ 10 TeV
Bounds from EM moments
10−2 10−1 100 101 102 Mχ = MB [TeV] 10−16 10−14 10−12 10−10 10−8 10−6 10−4 10−2 100 102 104 Rate, event / (kg·day)
Nf = 2 Nf = 6 XENON100 [1207.5988], 95% CL exclusion
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
★ baryon similar to QCD neutron ★ dark quarks with Q=Y ★ calculate connected 3pt ★ scale set by DM mass ★ magnetic moment dominates ★ results independent of Nf
[LSD, 1301.1693]
SU(3) Nf=2,6 dark fermionic baryon
Excluded MB >~ 10 TeV pushed to ~100 TeV with new LUX
Bounds from EM moments
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
★ dm is “mesonic” pNGB ★ calculate connected 3pt ★ use VMD with lattice ρ mass ★ scale set by Fπ=256 GeV ★ depends on isospin breaking dB ★ also couples to Higgs (d1+d2)
[Hietanen et al., 1308.4130]
SU(2) Nf=2 pNGB DM
super CDMS XENON100 LUX
10 100 50 20 200 30 300 15 150 70 10-46 10-45 10-44 10-43 10-42 10-41 10-40
DM mass, mf @GeVD DM-proton cross section, sp @cm2D dB=-0.1, d1+d2=1
[Plenary talk by Pica, Sat@09:00]
Bounds from EM moments
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
super CDMS LUX XENON100
10 100 50 20 200 30 300 15 150 70 10-46 10-45 10-44 10-43 10-42 10-41 10-40
DM mass, mf @GeVD DM-proton cross section, sp @cm2D dB=-1, d1+d2=1
★ dm is “mesonic” pNGB ★ calculate connected 3pt ★ use VMD with lattice ρ mass ★ scale set by Fπ=256 GeV ★ depends on isospin breaking dB ★ also couples to Higgs (d1+d2)
[Hietanen et al., 1308.4130]
SU(2) Nf=2 pNGB DM
[Plenary talk by Pica, Sat@09:00]
Bounds from EM moments
γ
Mesonic and Baryonic EM form factors directly from lattice simulations
[Plenary talk by Collins, Tue@10:15]
super CDMS LUX XENON100
10 100 50 20 200 30 300 15 150 70 10-46 10-45 10-44 10-43 10-42 10-41 10-40
DM mass, mf @GeVD DM-proton cross section, sp @cm2D dB=-1, d1+d2=1
★ dm is “mesonic” pNGB ★ calculate connected 3pt ★ use VMD with lattice ρ mass ★ scale set by Fπ=256 GeV ★ depends on isospin breaking dB ★ also couples to Higgs (d1+d2)
[Hietanen et al., 1308.4130]
SU(2) Nf=2 pNGB DM
MB ~< 13 GeV depends on dB Excluded
[Plenary talk by Pica, Sat@09:00]
Computing polarizability
Nucleus Nucleus
p p0 k k0 ` ` − q k + `
q = k0 − k = p − p0
cF e2 m3
↵vµv⌫
γ γ
[Weiner & Yavin,1206.2910] [Frandsen et al., 1207.3971] [Pospelov & Veldhuis, hep-ph/0003010] [Ovanesyan & Vecchi, 1410.0601] [Detmold et al., 0904.1586-1001.1131]
Computing polarizability
Nucleus Nucleus
p p0 k k0 ` ` − q k + `
q = k0 − k = p − p0
Lattice
cF e2 m3
↵vµv⌫
γ γ
[Weiner & Yavin,1206.2910] [Frandsen et al., 1207.3971] [Pospelov & Veldhuis, hep-ph/0003010] [Ovanesyan & Vecchi, 1410.0601] [Detmold et al., 0904.1586-1001.1131]
Computing polarizability
Nucleus Nucleus
p p0 k k0 ` ` − q k + `
q = k0 − k = p − p0
Lattice Nuclear Physics
cF e2 m3
↵vµv⌫
γ γ
[Weiner & Yavin,1206.2910] [Frandsen et al., 1207.3971] [Pospelov & Veldhuis, hep-ph/0003010] [Ovanesyan & Vecchi, 1410.0601] [Detmold et al., 0904.1586-1001.1131]
σnucleon(Z, A) = Z4 A2 144πα4µ2
nχ(M A F )2
m6
χR2
[cF ]2
Lowest bound from EM polarizability
Electric polarizability from lattice simulations with background fields
γ γ
[LSD, 1503.04205]
×- ×- ×- ×- ×- ×- χ()
SU(4) Nf=4 Stealth DM
[see also Drach et al.,1511.04370 for SU(2) Nf=2]
σnucleon(Z, A) = Z4 A2 144πα4µ2
nχ(M A F )2
m6
χR2
[cF ]2
Lowest bound from EM polarizability
Electric polarizability from lattice simulations with background fields
γ γ
[LSD, 1503.04205]
×- ×- ×- ×- ×- ×- χ()
LUX exclusion bound for spin-independent cross section
SU(4) Nf=4 Stealth DM
[see also Drach et al.,1511.04370 for SU(2) Nf=2]
σnucleon(Z, A) = Z4 A2 144πα4µ2
nχ(M A F )2
m6
χR2
[cF ]2
Lowest bound from EM polarizability
Electric polarizability from lattice simulations with background fields
γ γ
[LSD, 1503.04205]
×- ×- ×- ×- ×- ×- χ()
LUX exclusion bound for spin-independent cross section Coherent neutrino scattering background
SU(4) Nf=4 Stealth DM
[see also Drach et al.,1511.04370 for SU(2) Nf=2]
σnucleon(Z, A) = Z4 A2 144πα4µ2
nχ(M A F )2
m6
χR2
[cF ]2
Lowest bound from EM polarizability
Electric polarizability from lattice simulations with background fields
γ γ
[LSD, 1503.04205]
×- ×- ×- ×- ×- ×- χ()
LUX exclusion bound for spin-independent cross section Coherent neutrino scattering background LEPII bound on charged mesons
SU(4) Nf=4 Stealth DM
[see also Drach et al.,1511.04370 for SU(2) Nf=2]
σnucleon(Z, A) = Z4 A2 144πα4µ2
nχ(M A F )2
m6
χR2
[cF ]2
Lowest bound from EM polarizability
Electric polarizability from lattice simulations with background fields
γ γ
[LSD, 1503.04205]
lowest allowed direct detection cross-section for composite dark matter theories with EW charged constituents
×- ×- ×- ×- ×- ×- χ()
LUX exclusion bound for spin-independent cross section Coherent neutrino scattering background LEPII bound on charged mesons
SU(4) Nf=4 Stealth DM
[see also Drach et al.,1511.04370 for SU(2) Nf=2]
Concluding remarks
★QCD ideas and lattice QCD techniques can be borrowed when exploring the DM landscape (BSM) ★Composite dark matter is a viable interesting possibility with rich phenomenology ★Lattice methods can help in calculating direct detection cross sections, production rates at colliders, and self- interaction cross sections of phenomenological relevance. ★Dark matter constituents can carry electroweak charges and still the stable composites are currently undetectable. Stealth cross section.
extra
Open questions and future projects
scattering cross-section: hadron-hadron interactions are hard to model, but can be studied directly with lattice methods
need to know their form factors: lattice methods can be used
first order, gravitational wave signals could be soon
[Schwaller, 1504.07263]
A very familiar picture
[Wikipedia]
The Standard Model of particles
A very familiar picture
[Wikipedia]
The Standard Model of particles Mesons, Baryons and Glueballs
Confinement
Axion dark matter
with the Strong-CP problem
candidate
perturbative QCD input
CAST-IAXO (CERN) with large discovery potential in the next few years
Ωtot = 1.000(7) PDG 2014
[Preskill, Wise & Wilczek, Phys. Lett. B 120 (1983) 127-132] [Peccei & Quinn: PRL 38 (1977) 1440, PR D16 (1977) 1791]
10-10 10-16 10-15 10-14 10-13 10 100 1000 1 10 100 Axion Coupling |ga | (GeV-1) Axion Mass (µeV) 2015 2016 2017 2018 2019 " H a d r[ADMX]
Axion dark matter
with the Strong-CP problem
candidate
perturbative QCD input
CAST-IAXO (CERN) with large discovery potential in the next few years
Ωtot = 1.000(7) PDG 2014
[Preskill, Wise & Wilczek, Phys. Lett. B 120 (1983) 127-132]
Lattice Field Theory methods
[Peccei & Quinn: PRL 38 (1977) 1440, PR D16 (1977) 1791]
10-10 10-16 10-15 10-14 10-13 10 100 1000 1 10 100 Axion Coupling |ga | (GeV-1) Axion Mass (µeV) 2015 2016 2017 2018 2019 " H a d r[ADMX]
Constraints from lattice simulations
➥ compatible with model predictions, but large non-perturbative effects
well described by models? ➥ light fermions importantly affect the vacuum
[Bonati et al., 1512.06746] [Berkowitz, Buchoff, ER., 1505.07455]
m2
af 2 a = ∂2F
∂θ2
△ △ ◇ △ △ △ △ △ △△ △◇◇★ ★◇ ✶
1. 2. 3. 4. 5. 6. 0. 0.1 0.2 0.3 0.4 0.5 T/Tc χ1/4/Tc Nσ DIGM fit + statistical error △ 64 Systematic fitting error ◇ 80 ★ 96 ✶ 144χ T 4
c
= C (T/Tc)n
[Kitano&Yamada, 1506.00370][Borsanyi et al., 1508.06917][Frison et al.,1606.07175]
Non-perturbative calculation of QCD topology at finite temperature
[Trunin et al., 1510.02265][Petreczky et al., 1606.03145][Borsanyi et al., 1606.07494] [Talk by Katz, Mon.@14:35][Talk by Szabo, Mon.@13:15] [Talk by Frison, Mon.@14:35][Talk by Taniguchi, Fri.@17:10] [Talk by Martinelli, Fri@13:00]
Constraints from lattice simulations
➥ compatible with model predictions, but large non-perturbative effects
well described by models? ➥ light fermions importantly affect the vacuum
[Bonati et al., 1512.06746] [Berkowitz, Buchoff, ER., 1505.07455]
m2
af 2 a = ∂2F
∂θ2
△ △ ◇ △ △ △ △ △ △△ △◇◇★ ★◇ ✶
1. 2. 3. 4. 5. 6. 0. 0.1 0.2 0.3 0.4 0.5 T/Tc χ1/4/Tc Nσ DIGM fit + statistical error △ 64 Systematic fitting error ◇ 80 ★ 96 ✶ 144χ T 4
c
= C (T/Tc)n
[Kitano&Yamada, 1506.00370][Borsanyi et al., 1508.06917][Frison et al.,1606.07175]
Non-perturbative calculation of QCD topology at finite temperature
[Trunin et al., 1510.02265][Petreczky et al., 1606.03145][Borsanyi et al., 1606.07494]
Great effort to control all systematic lattice effects in order to impact experiments. This direction has started only 1 year ago!
[Talk by Katz, Mon.@14:35][Talk by Szabo, Mon.@13:15] [Talk by Frison, Mon.@14:35][Talk by Taniguchi, Fri.@17:10] [Talk by Martinelli, Fri@13:00]
Axion mass lower bound
[ADMX Website] [Berkowitz, Buchoff, ER., 1505.07455]
m2
af 2 a = ∂2F
∂θ2
Axion mass lower bound
Lattice SU(3) Pure Glue fa < (4.10±0.04) 1011 GeV ma > (14.6±0.1) μeV
[ADMX Website] [Berkowitz, Buchoff, ER., 1505.07455]
m2
af 2 a = ∂2F
∂θ2
Axion mass lower bound
Lattice SU(3) Pure Glue fa < (4.10±0.04) 1011 GeV ma > (14.6±0.1) μeV
[ADMX Website]
axions < 100% of DM smaller χ
[Berkowitz, Buchoff, ER., 1505.07455]
m2
af 2 a = ∂2F
∂θ2
Axion mass lower bound
Lattice QCD with physical quarks ma > (28±2) μeV
[ADMX Website] [Borsanyi et al., 1606.07494] [Talk by Katz, Mon.@14:35][Talk by Szabo, Mon.@13:15]
m2
af 2 a = ∂2F
∂θ2
[Talk by Frison, Mon.@14:35][Talk by Taniguchi, Fri.@17:10] [Talk by Martinelli, Fri@13:00]
Colliders
SUSY Stealth LSP heavier superpartners scalar baryon baryon excited resonances Collider searches dominated by light meson production and decay. Missing energy signals largely absent!
ρ Πs
Plot by G. Kribs
Composite DM signatures at colliders
VS.
Colliders
SUSY Stealth LSP heavier superpartners scalar baryon baryon excited resonances Collider searches dominated by light meson production and decay. Missing energy signals largely absent!
ρ Πs
Plot by G. Kribs
★ Signatures are not dominated by missing energy: DM is not
the lightest particle! The interactions are suppressed (form factors)
Composite DM signatures at colliders
VS.
Colliders
SUSY Stealth LSP heavier superpartners scalar baryon baryon excited resonances Collider searches dominated by light meson production and decay. Missing energy signals largely absent!
ρ Πs
Plot by G. Kribs
★ Signatures are not dominated by missing energy: DM is not
the lightest particle! The interactions are suppressed (form factors)
★ Light meson production and decay give interesting
signatures: the model can be constrained by collider limits
Composite DM signatures at colliders
VS.
Photon interactions
hχ(p0)|jµ
EM|χ(p)i = F(q2)qµ
✦dimension 5 ➥ magnetic dipole ✦dimension 6 ➥ charge radius ✦dimension 7 ➥ polarizability
(¯ χσµνχ)Fµν Λdark
(¯ χχ)vµ∂νF µν Λ2
dark
(¯ χχ)FµνF µν Λ3
dark
Expansion at low momentum through effective operators
[Bagnasco et al.,hep-ph/9310290]