long lived particles in susy...
TRANSCRIPT
Long Lived Particles in Viable SUSY Dark Matter Models
Satoshi Shirai (Kavli IPMU)
Based on
H. Fukuda, N. Nagata, H. Otono, and SS,“Probing bino–gluino coannihilation at the LHC,” Phys.Lett. B748 (2015) 24, “Probing bino–wino coannihilation at the LHC,” JHEP 1510 (2015) 086,“Cornering Compressed Gluino at the LHC,” JHEP 1703 (2017) 025,“Higgsino Dark Matter or Not,” Phys.Lett. B781 (2018) 306
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1. SUSY after LHCHiggs MassMini-split SUSYDark Matter
2. Dark Matter Signatures in Mini-SplitWinoGaugino coannihilationLong lived particle signatures
3. Summary
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Higgs and SUSY at LHC
Higgs Discovered! SUSY Constrained!
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Cornering Higgs and SUSY
Higgs Mass Range Squark Mass Limit
Year Year
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SUSY Higgs
In MSSM
This is clearly less than observed 125 GeV Higgs!
Higgs potential
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SUSY after 125 GeV Higgs
Scalar top
New InteractionSUSY
NMSSM“4-th” family
New Gauge Interaction
Large massA-term
Lambda SUSYFat higgs
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SUSY after 125 GeV Higgs
Scalar top
New InteractionSUSY
NMSSM“4-th” family
New Gauge Interaction
Large massA-term
Lambda SUSYFat higgs
Simple? Natural?
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Higgs Mass from Stop125 GeV Higgs OK regions
Scalar Mass
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Benefit and demerit of SUSY
• Hierarchy Problem• GUT unification• DM
Benefit
Possible demerit
• Flavor/CP Problem
• Cosmological Gravitino Problem
• Model building
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Mini-Split Mass Spectrum
Tree level Gravity Mediation
Loop suppressed: e.g., Anomaly Mediation
Randall, Sundrum ’98Giudice, Luty, Murayama, Rattazzi ’98
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Benefit and demerit of SUSY
• Hierarchy Problem• GUT unification• DM
Benefit
Possible demerit
• Flavor/CP Problem
• Cosmological Gravitino Problem
• Model building
?
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Three Possibilities for DM
wino
bino
gluino
binogluino
wino
Wino DM Bino-gluino coannihilation
binowino
gluino
Bino-wino coannihilation
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Wino DM case
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Wino Spectrum
Radiative correction
Charged slightly heavier [Ibe,Matsumoto,Sato 12]
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LHC Signals
p
p
gluon
O(1-10)cm
Meta-stable track+MET
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Current Constraint(wino)
3 cm
30 cm
MET + disappearing track
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Prospects for Wino
BG=10
BG=0
MET>400 GeV MET>600 GeV
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Three Possibilities for DM
wino
bino
gluino
binogluino
wino
Wino DM Bino-gluino coannihilation
binowino
gluino
Bino-wino coannihilation
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Bino-Gluino Coannihilation
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Bino-Gluino Coannihilation 1
1 TeV bino
Observed DM
Dark matter abundance
Gluino-bino mass difference
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Gluino Coannihilation
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LHC Signals
p
p
gluino
gluino bino
q q
bino
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Prompt Decay Case
Mass diff. = 100 GeV
Bino-Gluino Interaction
gluino bino
Bino-gluino interaction is suppressed by sfermion mass
Long-lived gluino
Too heavy sfermion prevents coannihilation
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Bino-Gluino Coannihilation
E.g.,For 100 TeV sfermion,
Mass diff. ~ 100 GeVDecay length ~ cm
Required mass difference
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Bino-Gluino Coannihilation 2
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P P
Displaced Vertex
tracks
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P P
Displaced Vertex
tracks
Missing energy
d0 > O(1) mm
invariant mass > 10 GeV
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ATLAS DV Search [ATLAS, PRD 97 052012]
13 TeV 32.8 fb-1• MET trigger + event filer > 250 GeV
• DV with impact parameter > 2 mm
• Mass of DV > 10 GeV
• # of tracks >4
without DV BG O(10^5)
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Bino-Gluino Interaction
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Prospects
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Bino-Gluino Prospects
DV
dE/dx
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Three Possibilities for DM
wino
bino
gluino
binogluino
wino
Wino DM Bino-gluino coannihilation
binowino
gluino
Bino-wino coannihilation
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Bino-Wino Coannihilation
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Bino-Wino Coannihilation
A few tens of GeV mass diff.
Required mass difference
LHC SignalsMass diff. 30 GeV
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Wino Decay (tree)
Suppressed by Higgsino mass
Small Yukawa
Long-lived neutral wino
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Prompt charged Wino decay
Displaced neutral Wino decay
Wino Decay
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Wino Decay Bino = 400 GeVWino = 430 GeV
Higgs mass OK
Decay length of neutral wino
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LHC Signals
p
pbino
b b
bino
Low mass ~ 10 GeV DV+MET
gluon
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LHC Prospects
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Summary
Mini-split is simplest SUSY model with 125 GeV Higgs
DM in mini-split likely provide meta-stable particles● Wino DM: disappering track● Gluino-bino DM: long-lived R-hadron● Wino-bino DM: long-lived neutral wino
Improvement of LLP detection