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The Reach of Thermal Supersymmetric Dark Matter The Reach of Thermal Supersymmetric Dark Matter Jason L. Evans Korea Institute for Advanced Study The Reach of Thermal Supersymmetric Dark Matter Outline Motivations SUSY Dark Matter
The Reach of Thermal Supersymmetric Dark Matter
Jason L. Evans
Korea Institute for Advanced Study
The Reach of Thermal Supersymmetric Dark Matter
Motivations SUSY Dark Matter Coannihillation Gluino Coannihilation Stop Coannihilation
The Reach of Thermal Supersymmetric Dark Matter Motivations
◮ SUSY is most likely somewhat tuned − ∆BG ∼ M2
SUSY/m2 Z
◮ Is it time to let that ship sink? − We worry because we can detect it
Mass Scale [GeV] 200 400 600 800 1000 1200 1400 1600 1800 2000
1 χ ∼ 1 χ ∼ W Z → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ W H → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ W Z → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ ν τ τ τ → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ ν τ ll → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ ν lll → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ 1 χ ∼ ν lll → 1 ± χ ∼ 2 χ ∼ → pp 1 χ ∼ q → q ~ , q ~ q ~ → pp 1 χ ∼ q → q ~ , q ~ q ~ → pp 1 χ ∼ b → b ~ , b ~ b ~ → pp 1 χ ∼ b → b ~ , b ~ b ~ → pp 1 χ ∼ b → b ~ , b ~ b ~ → pp 1 χ ∼ b → b ~ , b ~ b ~ → pp 1 χ ∼ ± b W → b ± 1 χ ∼ → t ~ , t ~ t ~ → pp 1 χ ∼ ± b W → b ± 1 χ ∼ → t ~ , t ~ t ~ → pp 1 χ ∼ ± b W → b ± 1 χ ∼ → t ~ , t ~ t ~ → pp 1 χ ∼ ± b W → b ± 1 χ ∼ → t ~ , t ~ t ~ → pp (4-body) 1 χ ∼ b f f → t ~ , t ~ t ~ → pp (4-body) 1 χ ∼ b f f → t ~ , t ~ t ~ → pp (4-body) 1 χ ∼ b f f → t ~ , t ~ t ~ → pp 1 χ ∼ c → t ~ , t ~ t ~ → pp 1 χ ∼ c → t ~ , t ~ t ~ → pp 1 χ ∼ c → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ t → t ~ , t ~ t ~ → pp 1 χ ∼ qq (W/Z) → ) 2 χ ∼ / 1 ± χ ∼ qq( → g ~ , g ~ g ~ → pp 1 χ ∼ qq (W/Z) → ) 2 χ ∼ / 1 ± χ ∼ qq( → g ~ , g ~ g ~ → pp 1 χ ∼ qq W → 1 ± χ ∼ qq → g ~ , g ~ g ~ → pp 1 χ ∼ qq W → 1 ± χ ∼ qq → g ~ , g ~ g ~ → pp 1 χ ∼ qq W → 1 ± χ ∼ qq → g ~ , g ~ g ~ → pp 1 ± χ ∼ bt → g ~ , g ~ g ~ → pp 1 χ ∼ t c → t ~ t → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ tt → g ~ , g ~ g ~ → pp 1 χ ∼ bb → g ~ , g ~ g ~ → pp 1 χ ∼ bb → g ~ , g ~ g ~ → pp 1 χ ∼ bb → g ~ , g ~ g ~ → pp 1 χ ∼ qq → g ~ , g ~ g ~ → pp 1 χ ∼ qq → g ~ , g ~ g ~ → pp EWK Gauginos < 40 GeV) LSPSelected CMS SUSY Results* - SMS Interpretation Moriond '17
= 13TeV s CMS Preliminary
L = 12.9 fb
L = 35.9 fb
LSPm ⋅ +(1-x)
Motherm ⋅ = x
Intermediatem For decays with intermediate mass, 0 GeV unless stated otherwise ≈
LSPOnly a selection of available mass limits. Probe *up to* the quoted mass limit for m *Observed limits at 95% C.L. - theory uncertainties not included
The Reach of Thermal Supersymmetric Dark Matter Motivations
◮ Gauge couplings unify in SUSY ◮ MGUT affects on Unification − MGUT thresholds → unification ◮ Unification → upper limit on MSUSY − β(αi) change at MSUSY − µ, Mi ≫ mW → no unification
SUSY
M
GUTM
1 1
1 2
1 3
1 5
f ~ ~
CH
8 , 3
Minimal SU(5)
X
The Reach of Thermal Supersymmetric Dark Matter SUSY Dark Matter
◮ WIMP miracle − Weak scale masses/interactions give correct density ◮ Netralinos: the perfect WIMP (r = M2
1/m2 ˜ eR → 0.25)
− density only depends on scattering cross section
σ˜
Bv = 3g3t3 wr(1 + r 2)
2πm2
˜ eR x(1 + r)4
σeff˜
H v ≃
21g4 512πµ2
σeff ˜
W v =
3g4 16πM2
2
Ωh2 ≃ 0.12
eR
100 GeV 2 Ω˜
Hh2 ≃ 0.1
1 TeV
2 Ω ˜
W h2 ≃ 0.13
2.5 TeV 2
The Reach of Thermal Supersymmetric Dark Matter SUSY Dark Matter
◮ WIMP miracle − Weak scale masses/interactions give correct density ◮ Netralinos: the perfect WIMP (r = M2
1/m2 ˜ eR → 0.25)
− density only depends on scattering cross section − Thermal Wino ruled out?
σ˜
Bv = 3g3t3 wr(1 + r 2)
2πm2
˜ eR x(1 + r)4
σeff˜
H v ≃
21g4 512πµ2
σeff ˜
W v =
3g4 16πM2
2
Ωh2 ≃ 0.12
eR
100 GeV 2 Ω˜
Hh2 ≃ 0.1
1 TeV
2 Ω ˜
W h2 ≃ 0.13
2.5 TeV
2
The Reach of Thermal Supersymmetric Dark Matter SUSY Dark Matter
◮ WIMP miracle − Weak scale masses/interactions give correct density ◮ Netralinos: the perfect WIMP (r = M2
1/m2 ˜ eR → 0.25)
− density only depends on scattering cross section − Thermal Wino ruled out?(Cohen,Lisanti,Pierce,Slatyer)
0.5 1.0 1.5 2.0 2.5 3.0 104 103 103 102 102 101 101 1 10 10 M2 TeV Dark Matter Fraction
The Reach of Thermal Supersymmetric Dark Matter SUSY Dark Matter
◮ WIMP miracle − Weak scale masses/interactions give correct density ◮ Netralinos: the perfect WIMP (r = M2
1/m2 ˜ eR → 0.25)
− density only depends on scattering cross section − Thermal Wino ruled out? ◮ Simple thermal relics all but gone (Badziak, Olechowski, Szczerbiak)
Red: LUX(SI), Green: LUX(SD), Orange: (XENON1T), Yellow: (LZ)
200 400 600 800 1000
mLSP [GeV]
2 3 4 5 6 7 8 9 10 11 12 13 14 15
tanβ
LZ XENON1T N 2
11 =0.580% 120% 1 2 5 50 200 7 9 Ωh2 ≈0.12, µM1 <0 200 400 600 800 1000
mLSP [GeV]
2 3 4 5 6 7 8 9 10 11 12 13 14 15
tanβ
LZ XENON1T N 2
11 =0.5Ωh2 ≈0.12, µM1 >0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation
χ ˜ t1 SM SM χ, ˜ t1 χ, ˜ t1 SM SM
◮ Reaction rates nχn˜
t1σχ˜ t1 ∼ T 3m3/2 χ m3/2 ˜ t1 σχ˜ t1e
mχ+m˜ t1 T
t1SM ∼ T 9/2m3/2 χ σχSMe
T
m˜
t1
3/2 exp m˜
t1
T
− Thermal Fluctuations convert LSP to NSLP ◮ As ˜ t1 annihilates, replenished by SM scattering − n˜
t1eq ≃ nχeq → enhances σχχeff.
◮ Scattering of coannihilation partner determines density
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Gluino coannihilation largest Sommerfeld enhancement − Final states: singlet, octet, and 27s for Cj = 0, 3, 8 − Stronger binding energy more enhancement V = αs 2r
i
− R hadron production enhances ˜ g˜ g annihilation rate − Γ˜
R ≫ Γdis enhanced coannihilation
σv˜
g˜ g→gg,q¯ q → σv˜ g˜ g incl. ˜ R ≡ σv˜ g˜ g→gg,q¯ q + σvbsf
Γ˜
R
Γ˜
R + Γdis
,
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Relative importance of Sommerfeld and Bound state − No Som/Boun (red) Som only (Orange) − All (Black) Boun×2 (Purple)
2000 4000 6000 8000 10000 50 100 150 200
mΧGeV mg
mΧGeV
mq
mg 50 Ellis,Luo,Olive
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Relative importance of Sommerfeld and Bound state ◮ Somewhat insensitive to squark mass − Squark mass control conversion of ˜ χ ↔ ˜ g
1 10 100 5 50 500 2000 4000 6000 8000 10000
mq
mΧ
mΧGeV
Ellis,Luo,Olive
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Non-universal input gauginos → gluino coannihilation − Gluino coannihilation extends to mχ ∼ 8.5 TeV M1 = M2, M3, m0, tan β, A0
1.0×102 1.0×104 1.6×104 1000 2000 3000 1.0×102 1.0×104 1.6×104 1000 2000 3000
M 3 (GeV) M 1 (GeV)
tan β = 3, A0 = 1.5 m0, m0 = 200 TeV, µ > 0
1000 2000 3000 100 200
M3 (GeV) ΔM (GeV)
5 10
mχ (TeV)
tan β = 3, A0 = 1.5 m0, m0 = 200 TeV, µ > 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Pure-Gravity Mediation − GM term → linearly independent B, µ → free tan β m0, tan β ◮ Gauginos mass anomaly mediated Mi = bi g2
i
16π2 m3/2 bi = 33 5 , 1, −3
10 mass from GM term − Additional 10 can couple to Hu → larger tan β, mh K ⊃ cH10¯ 10 + h.c W ⊃ y ′
t HuQ′U′ + ..
− Gaugino mass do not decouple − Gluino mass purely from thresholds M1 = 48 5 g2
1
16π2 m3/2 M2 = g2
2
4π2 m3/2 M3 = 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Gluino Coannihilation
◮ Gluino coannihilation extends to mχ ∼ 8.5 TeV − For smaller cH gluino thresholds small and ˜ g is LSP
0.12 0.2 0.22
122 123 124 1 2 5 1 2 5 125 126 126 1260.12 0.2 0.2 30 100 200 400 600
125 124 GeV
tan β = 3, yt´2 = 0.15
m3/2 (TeV) cH
126 123 122
100 200
ΔM (GeV)
5 10
mχ (TeV) m3/2 (TeV)
tan β = 3, yt´2 = 0.15
30 100 600 200 400
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Stop coannihilation is also Sommerfeld enhanced − Final states: singlet or octet for Cf = 0, 3 − Less enhanced compared to gluino case (C3 = 4
3)
V = αs 2r
i
− Octet ˜ tR˜ t∗
R forms bound state from gluino emission ǁ 𝑢𝑆 ǁ 𝑢𝑆
∗
g 8 8
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Stop coannihilation is also Sommerfeld enhanced − Final states: singlet or octet for Cj = 0, 3 − Less enhanced compared to gluino case (C3 = 4
3)
V = αs 2r
i
− Octet ˜ tR˜ t∗
R forms bound state from gluino emission
− Γ˜
R ≫ Γdis enhanced coannihilation
σv˜
t˜ t∗→SM → σv˜ t˜ t∗ incl. ˜ R ≡ σv˜ t˜ t∗→SM + σvbsf
Γ˜
R
Γ˜
R + Γdis
,
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Goldstone Boson Equivalence Theorem (GBET) − WL/ZL remember origins ◮ GBET leads to enchanced t → Wb decay rate − Goldstone couples via top Yukawa (yt > g2) Γt ≃ g2
2
64π m3
t
m2
W
= y2
t
32πmt ◮ In SUSY stops couple to goldstone via A-terms − At ≫ MSUSY, large enhancement to WL/ZL couplings − Goldston predominantly in the Hu, only At matters L ⊃ −yt(AtHu + µH†
d) ˜
QL˜ tR − |yt|2 | ˜ QL|2|Hu|2 + |˜ tR|2|Hu|2|
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ In Feynman gauge goldstone boson are manifest − ˜ tR˜ t∗
R → W +W −
≃ ˜ tR˜ t∗
R → G+G−
L ⊃ −ytXt sin βG+˜ bL˜ tR − |yt|2 sin2 β|˜ tR|2|G+|2
ǁ 𝑢𝑆 𝐻+ 𝐻+ 𝐻+ 𝐻+ ǁ 𝑢𝑆 ǁ 𝑢𝑆
∗
ǁ 𝑢𝑆
∗
෨ 𝑐𝑀
◮ s-wave annihillation two sources of enhancement − yt > g2 and At >
tR + m2 tL
− For At/
tR + m2 tL g3/yt, most important mode
σv˜
t˜ t∗→W +W − ≃
g4
2
128πm2
˜ tR
mt mW 4 (At + µ cot β)2 − m2
˜ tR − m2 ˜ tL
m2
˜ tR + m2 ˜ tL
2
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ For large At, mχ ∼ 8 TeV (Similar to gluino case)
− m0 chosen to give relic density Solid (All) Dashed (No BS) Dash-Dot (No GS) Solid (µ < 0)
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120
m1/2 (TeV) δm (GeV)
1 2 3 4 5 6 7 8 9 20 40 60 80 100 120
A0 = 3m0, tan β = 20
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120
m1/2 (TeV) δm (GeV)
1 2 3 4 5 6 7 8 9 20 40 60 80 100 120
A0 = 5m0, tan β = 20
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ For large At, mχ ∼ 8 TeV (Similar to gluino case) ◮ At < 0, mχ ∼ 3 TeV
− |At(MSUSY)| ≪ MSUSY due to RG running Solid (All) Dashed (No BS) Dash-Dot (No GS) Solid (µ < 0)
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120
m1/2 (TeV) δm (GeV)
1 2 3 4 5 6 7 8 9 20 40 60 80 100 120
A0 = 3m0, tan β = 20
1 2 3 4 5 6 7 8 10 20 30 40 50 60
m1/2 (TeV) δm (GeV)
1 1.5 2 2.5 3 3.5 10 20 30 40 50 60
A0 = −4.2m0, tan β = 20
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ For large At, mχ ∼ 8 TeV (Similar to gluino case) ◮ At < 0, mχ ∼ TeV (Similar to gluino case)
− |At(MSUSY)| ≪ MSUSY due to RG running
◮ Little dependence on tan β − Some enhancement from µ for small tan β
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120
m1/2 (TeV) δm (GeV)
A0, tb = −4.2, 5 A0, tb = −4.2, 20 A0, tb = −4.2, 30 A0, tb = 3, 5 A0, tb = 3, 20 A0, tb = 3, 30 1 2 3 4 5 6 7 8 9 20 40 60 80 100 120
A0/m0 = −4.2, 3; µ > 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Higgs mass constrain coannihilation strip − A0 < 0, |At| is small and Higgs mass resonable
1 2 3 4 5 6 7 8 10 20 30 40 50 60
m1/2 (TeV) δm (GeV)
1 2 3 4 5 6 7 8100 105 110 115 120 125 130 135
mh (GeV)
m˜
t − mχ
SSARD SUSYHD FH2100 FH2130OS FH2130DR 1 1.5 2 2.5 3 3.5
A0 = −4.2m0, tan β = 5, µ > 0
1 2 3 4 5 6 7 8 10 20 30 40 50 60
m1/2 (TeV) δm (GeV)
1 2 3 4 5 6 7 8100 105 110 115 120 125 130 135
mh (GeV)
m˜
t − mχ
SSARD SUSYHD FH2100 FH2130OS FH2130DR 1 1.5 2 2.5 3 3.5
A0 = −4.2m0, tan β = 5, µ < 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Higgs mass constrain coannihilation strip − A0 > 0 and At large, Higgs mass calculation unstable
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120 140
m1/2 (TeV) δm (GeV)
2 4 6 8 10 12 14 16 18 30 40 50 60 70 80 90 100 110 120 130
mh (GeV)
m˜
t − mχ
SSARD SUSYHD FH2100 FH2130OS FH2130DR 1 2 3 4 5 6 7 8
A0 = 3m0, tan β = 20, µ > 0
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120 140
m1/2 (TeV) δm (GeV)
2 4 6 8 10 12 14 16 18 70 80 90 100 110 120 130
mh (GeV)
m˜
t − mχ
SSARD SUSYHD FH2100 FH2130OS FH2130DR 1 2 3 4 5 6 7 8
A0 = 3m0, tan β = 20, µ < 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Higgs mass constrain coannihilation strip − FeynHiggs 2.14.0 makes things worse
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120 140
m1/2 (TeV) δm (GeV)
2 4 6 8 10 12 14 16 18 20 40 60 80 100 120 140 160
mh (GeV)
m˜
t − mχ
SSARD SUSYHD FH2100 FH2130OS FH2130DR FH2140 1 2 3 4 5 6 7 8
A0 = 3m0, tan β = 20, µ > 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Higgs mass constraints coannihilation strip − FeynHiggs 2.14.0 makes things worse
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Corrections to Higgs quartic coupling (Mass) − Higgs mass suppressed for very large At
∆λ ⊃ |yt|4 8π2
Xt ˜ F1
tL
m˜
tR
12 ˜ X 2
t ˜
F2
tL
m˜
tR
Xt = At + µ cot β m˜
tRm˜ tL
◮ Coannihilation leading contribution − Coannihilation strip extended for large At
σv˜
t˜ t∗→W +W − ≃
g4
2
128πm2
˜ tR
mt mW 4 (At + µ cot β)2 − m2
˜ tR − m2 ˜ tL
m2
˜ tR + m2 ˜ tL
2
◮ Length of stop strip maximized for m˜
tR = m˜ tL
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Supersymmetry input scale may be below MGUT − Mirage mediation → apparent sub-GUT spectrum ◮ Smaller Min leads to less RG running − Stop masses less split − Higgs mass less suppressed − Coannihilation strip extended ◮ Use FeynHiggs 2.13.0 OS for Higgs mass calculation − Most recent available code at the time − FeynHiggs 2.14.0 now available but seems worse
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Sub-GUT models very different from CMSSM planes − Stop masses more split − Higgs mass much better
2 4 6 8 10 12 14 16 5 10 15 20
m1/2 (TeV) M (TeV)
˜ t1 mχ ˜ t2 ˜ t1 m
χ
˜ t2 Sub-GUT CMSSM
2 4 6 8 10 12 14 16 90 100 110 120 130
mh (GeV)
mh mh
A0 = 2.75m0, tanβ = 20, µ > 0
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Sub-GUT models very different from CMSSM planes ◮ Sub-GUT plane − Stop LSP region limited − Coannihilation region much less tuned
5.0×102 1.0×104 0.0 1.0×104 1.5×104
0.01 0.05 122 1 2 2 1 2 2 1 2 3 1 2 3 123 124 1 2 4 1 2 4 125 125 125 126 126 126 127 127 1 2 8 1285.0×102 1.0×104 0.0 1.0×104 1.5×104 129
m1/2 (GeV) m0 (GeV)
128
A0/m0 = 2.75, tan β = 20, μ < 0
127 130 122
Min = 109 GeV
5.0×102 1.0×104 0.0 1.0×104 1.5×104
. 1 122 123 124 1 2 4 1 2 5 1 2 5 125 125 126 126 1 2 6 127 127 1 2 8 1285.0×102 1.0×104 0.0 1.0×104 1.5×104 129
m1/2 (GeV) m0 (GeV)
128
A0/m0 = 2.75, tan β = 20, μ > 0
127 122
Min = 109 GeV
The Reach of Thermal Supersymmetric Dark Matter Coannihillation Stop Coannihilation
◮ Naturalness somewhat strained − But not dead ◮ Gauge coupling unification still good − Upper limit on SUSY breaking scale ∼ 106 GeV ◮ Thermal dark matter still alive − Gluino coannihilation extends to mχ 8.5 TeV − Stop coannihilation may extends to mχ 8.5 TeV − Sub-GUT models give more natural coannihilation