Collider Studies of Viable SUSY Dark Matter
Satoshi Shirai (Kavli IPMU) Based on H. Fukuda, N. Nagata, H. Oide, 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 “TBA”, to appear 1. WIMP Dark Matter 2. Current Status of SUSY Higgs Mass, direct detection Dark Matter candidates 3. Dark Matter Signatures Wino Higgsino Gaugino coannihilation 4. Summary
2 WIMP Dark Matter
3 DM Candidates
• Axion
• (Primordial) Black hole
• WIMP
• Others…
4 WIMP Dark Matter
Weakly Interacting Massive Particle
DM abundance DM Standard Model (SM) particle 500 GeV DM
DM SM
Time 5 WIMP Miracle
6 WIMP Detection
WIMP annihilation; Cosmic ray, CMB, BBN CTA (Cherenkov Telescope Array)
DM SM
WIMP scattering XMASS, XENONnT
DM SM
WIMP Production; Collider LHC, ILC
7 Collider Signals of DM
p, e- DM
DM is invisible
p, e+ DM
8 Collider Signals of DM
p, e- DM
DM is invisible
p, e+ DM Additional objects are needed to see DM. Missing energy (MET) search
9 DM Search at LHC
DM search is not easy
● Production rate of DM is tiny about 12 order magnitude smaller than SM
● Some SM events are very similar to DM signatures
Huge Background
10 Which is DM signature?
6.05
11 Which is DM signature? DM signal
6.05
12 Mono-jet Signatures
350 GeV WIMP (wino)
O(105) particle productions are required to see the signals 13 Example: Higgsino DM
Higgsino DM constraints (lower bound on Mass) based on missing energy:
90 GeV (2002, LEP2) 120 GeV (2018, LHC) 150 GeV (2030?, HL-LHC)
c.f., Scalar quark
330 GeV (2006, Tevatron) 1550 GeV (2018, LHC) 3000 GeV (2030?, HL-LHC)
Efficient BG reduction and/or new observable are needed
14 SUSY
15 SUSY Standard Model
Standard Model (SM) SUSY Partner Lepton Scalar Lepton Quark Scalar Quark Scalar Higgs Higgsino Gauge Boson Gaugino gluon gluino weak boson wino photon bino
Neutralino Dark Matter = mixture of wino + bino + Higgsino 16 Higgs and SUSY at LHC
Higgs Discovered! SUSY Constrained!
17 Cornering Higgs and SUSY
Higgs Mass Range Squark Mass Limit
Year Year
18 SUSY Higgs
Higgs potential
In MSSM
This is clearly less than observed 125 GeV Higgs!
19 SUSY after 125 GeV Higgs
SUSY New Interaction
Scalar top “4-th” family NMSSM Lambda SUSY Large mass Fat higgs A-term New Gauge Interaction
20 SUSY after 125 GeV Higgs
SUSY New Interaction
Scalar top “4-th” family NMSSM Lambda SUSY Large mass Fat higgs A-term New Gauge Interaction
Simple? Natural?
21 Higgs Mass from Stop 125 GeV Higgs OK regions
Scalar Mass
22 Direct Detection
Cross Section is proportional to the neutralino mixing parameter
Almost pure gaugino or Higgsino is preferred 23 Possibilities for DM
With 125 GeV Higgs mass and Direct detection constraint prefer
● Almost pure Wino
● Almost pure Higgsino
● Gaugino coannihilation ● bino-gluino mass degeneration ● bino-wino mass degeneration ● …
24 Wino DM case
25 Wino Property
• Majorana fermion
• Hypercharge Y=0
• SU(2)L triplet
• Mass < 3 TeV [Hisano, Matsumoto, Nagai, Saito & Senami, 06] 26 Wino Spectrum
Radiative correction
Charged slightly heavier [Ibe,Matsumoto,Sato 12]
27 LHC Signals
p
Meta-stable track + MET p
gluon
O(1-10)cm
28 Event Display
29 Event Display
30 Current Constraint(wino)
30 cm
3 cm
MET + disappearing track
31 Prospects for Wino
MET>400 GeV MET>600 GeV
BG=10 Tracking improvement
BG=0
[H. Fukuda, N. Nagata, H. Otono, and SS, `18]
32 Higgsino DM case
33 What is Higgsino?
Higgsino is
(pseudo)Dirac fermion
Hypercharge |Y|=1/2
SU(2)doublet
<1 TeV Pure Higgsino Spectrum
Radiative correction Higgsino Spectrum (with heavier gaugino) Current Constraint(higgsino)
disappearing track
37 Current Constraint(higgsino)
XENON1T
disappearing track
38 Current Constraint(higgsino)
XENON1T
Blind Spot disappearing track
39 Event Display
40 [H. Fukuda, H. Oide, H. Otono, and SS, `19] Current Constraint(higgsino)?
XENON1T
soft tracks improved disappearing track
41 Bino-Gluino Coannihilation
N. Nagata, H. Otono, and SS, ‘15&’17]
42 Gaugino coannihilation
wino gluino
gluino wino bino bino
Bino-gluino Bino-wino coannihilation coannihilation
43 Bino-Gluino Coannihilation 1
Dark matter abundance
Observed DM
1 TeV bino
Gluino-bino mass difference
44 Gluino Coannihilation
45 LHC Signals
q q
p gluino bino
p gluino bino
q q
46 Prompt Decay Case
Mass diff. = 100 GeV
47 Bino-Gluino Interaction
gluino bino
Bino-gluino interaction is suppressed by sfermion mass
Long-lived gluino Displaced Vertex
P P
tracks
49 Displaced Vertex
P P
d0 > O(1) mm
tracks
Missing energy
invariant mass > 10 GeV 50 Prospects
51 Bino-Wino Coannihilation
[N. Nagata, H. Otono, and SS, `16]
52 Bino-Wino Coannihilation
Required mass difference
A few tens of GeV mass diff. 53 LHC Signals Mass diff. 30 GeV Wino Decay (tree)
Small Yukawa
Long-lived neutral wino
Suppressed by Higgsino mass
55 Wino Decay
Prompt charged Wino decay
Displaced neutral Wino decay
56 Wino Decay Bino = 400 GeV Wino = 430 GeV
Higgs mass OK
Decay length of neutral wino
57 LHC Signals q q
p bino
Low mass ~ 10 GeV DV + MET p bino gluon b b
58 LHC Prospects
59 Summary
Mini-split is simplest SUSY model with 125 GeV Higgs
SUSY DMs likely provide meta-stable particles ● Wino, Higgsino DM: disappering track, soft tracks ● Gluino-bino DM: long-lived R-hadron ● Wino-bino DM: long-lived neutral wino
Improvement of LLP detection
60