Sho IWAMOTO. 7 Nov HEP phenomenology joint Cavendish DAMTP U. Cambridge

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1 MSSM scenario Sho IWAMOTO 7 Nov HEP phenomenology joint Cavendish DAMTP U. Cambridge Based on [ ] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine)

2 The Standard Model of Particle Physics Universe = Image by MissBJ [CC BY 3.0], via Wikimedia Commons 2 /70

3 The Standard Model of Particle Physics Universe = dark matter? 3 /70

4 The Standard Model of Particle Physics Universe = dark energy? dark matter? 4 /70

5 Physics beyond the Standard Model Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 5 /70

6 Physics beyond the Standard Model New Physics Candidates etc Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 6 /70

7 Physics beyond the Standard Model New Physics Candidates SUSY [supersymmetry] etc Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 7 /70

8 Physics beyond the Standard Model New Physics Candidates SUSY [supersymmetry] etc Please fill this list with your models / models you like Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 8 /70

9 Physics beyond the Standard Model New Physics Candidates SUSY [supersymmetry] Gauge-Higgs unification Hidden strong SU(N) etc Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 9 /70

10 Physics beyond the Standard Model New Physics Candidates SUSY Gauge-Higgs unification Hidden strong SU(N) etc Hints of New Physics Dark matter Dark energy c Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon /70

11 Physics beyond the Standard Model MSSM = [Standard Model] Image by MissBJ [CC BY 3.0], via Wikimedia Commons (changes were made by S.I) 11 /70

12 Physics beyond the Standard Model MSSM = [Minimal Supersymmetric Standard Model] Image by MissBJ [CC BY 3.0], via Wikimedia Commons (changes were made by S.I) 12 /70

13 Physics beyond the Standard Model New Physics Candidates SUSY Hints of New Physics Dark matter Dark energy c Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon /70

14 Physics beyond the Standard Model New Physics Candidates SUSY Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon /70

15 Gauge coupling unification SM 3 forces : U(1), SU(2), SU(3) Hints [Why of New three?] Physics Dark matter measured theoretical prediction Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... Figure from S. P. Martin, A Supersymmetry Primer, hep-ph/ /70

16 Gauge coupling unification SM 3 forces : U(1), SU(2), SU(3) Hints [Why of New three?] Physics Dark matter measured theoretical prediction Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... Figure from S. P. Martin, A Supersymmetry Primer, hep-ph/ /70

17 Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least yr) charge neutral density not detected by astrophysics / direct search / LHC 17 /70

18 Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least yr) charge neutral density not detected by astrophysics / direct search / LHC 18 /70

19 Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least yr) charge neutral density not detected by astrophysics / direct search / LHC 19 /70

20 Neutralino relic density overabundant problem 20 /70

21 Neutralino relic density overabundant problem MSSM model 21 /70

22 O u t l i n e Abdullah, Feng, SI, Lillard [ ] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 22 /70

23 Bino relic density Early Universe with pair creation equilibrium pair annihilation 23 /70

24 Bino relic density Early Universe with pair creation equilibrium pair annihilation 24 /70

25 Bino relic density Early Universe with pair creation pair annihilation far apart due to pair annihilation Universe s expansion relic density 25 /70

26 Bino relic density observed relic density proper crosssection of (DM)(DM) SM Figure from Gelmini and Gondolo, /70

27 Bino relic density observed relic density proper crosssection of (DM)(DM) SM pure -DM (i.e., LSP is -like) strongly depends on 27 /70

28 Co-annihilation An old solution to increase : co-annihilation mass splitting 28 /70

29 Co-annihilation An old An solution example to increase CMSSM with : co-annihilation -coann.: mass splitting Figure from Edsjö, Schelke, Ullio, Gondolo, hep-ph/ /70

30 O u t l i n e Abdullah, Feng, SI, Lillard [ ] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 30 /70

31 MSSM4G outline MSSM = 3Generations extra vector-like 4 th -Generation lepton MSSM4G Image by MissBJ [CC BY 3.0], via Wikimedia Commons (changes were made by S.I) 31 /70

32 MSSM4G outline A new solution to increase : MSSM4G extra annihilation channel larger proper if 32 /70

33 MSSM4G outline [MSSM] [MSSM4G] [vector-like mass] [mixing with SM leptons] 33 /70

34 MSSM4G : Two models MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification SU(5) GUT extra interaction m h QDEE model : MSSM + gauge coupling unification SU(5) GUT extra coupling m h slightly 34 /70

35 MSSM4G : Two models MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra interaction mh QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra coupling mh slightly 35 /70

36 MSSM4G : Working assumption (the minimal setup) MSSM + QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra breaks coupling unification interaction mh assumed to be decoupled (very heavy) and we will ignore them. coupling mh slightly Other working assumptions LSP is -like All the other SUSY particles & extra Higgses are decoupled. 36 /70

37 MSSM4G : Working assumption (the minimal setup) MSSM + QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra breaks coupling unification interaction mh assumed to be equal-mass coupling mh slightly Other working assumptions assumed to be equal-mass LSP is -like All the other SUSY particles & extra Higgses are decoupled. assumed to be equal-mass 37 /70

38 MSSM4G : Two models QUE model QDEE model Abdullah, Feng [ ] color bands show 38 /70

39 MSSM4G : Two models QUE model QDEE model Abdullah, Feng [ ] color bands show vanilla stau-coann. QUE QDEE 39 /70

40 O u t l i n e Abdullah, Feng, SI, Lillard [ ] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 40 /70

41 Constraints from cosmic-ray observations DM indirect detection (= searches for DM annihilation) DM DM DM DM time 41 /70

42 Constraints from cosmic-ray observations DM indirect detection (= searches for DM annihilation) DM DM DM DM time 42 /70

43 Constraints from cosmic-ray observations DM indirect detection (= searches for ) DM DM [vector-like mass] [mixing with SM leptons] 43 /70

44 Constraints from cosmic-ray observations DM indirect detection DM DM 44 /70

45 Constraints from cosmic-ray observations DM indirect detection DM DM insensitive (IceCube) less sensitive / large BKG uncertainty 45 /70

46 σ - ( / ) Gamma-ray searches in QUE models ~ ( ) Abdullah, Feng, SI, Lillard [ ] valid for any mixing patterns MSSM4G region MAGIC: 158 hr of Segue 1 Fermi-LAT: 6 yr of 15 dsph (incl. Segue 1) DM profile: NFW Fermi-LAT dominates MAGIC in almost all E-range. ( ) CTA prospect : 500hr of Milky Way DM profile: Einasto No syst. unc. (stat only) 46 /70

47 σ - ( / ) σ - ( / ) Gamma-ray searches in QUE models WW (any mixing pattern) ~ ( ) Abdullah, Feng, SI, Lillard [ ] ττ (only for τ-mixing cases) ~ ( ) τ + τ - - ( ) ( ) τ-mixing fully covered e/μ-mixing with > GeV covered MAGIC: 158 hr of Segue 1 Fermi-LAT: 6 yr of 15 dsph (incl. Segue 1) DM profile: NFW Fermi-LAT dominates MAGIC in almost all E-range. CTA prospect : 500hr of Milky Way DM profile: Einasto No syst. unc. (stat only) 47 /70

48 σ - ( / ) σ - ( / ) Gamma-ray searches in QDEE models WW (any mixing pattern) ~ ( ) Abdullah, Feng, SI, Lillard [ ] ττ (only for τ-mixing cases) ~ ( ) τ + τ - - ( ) ( ) τ-mixing fully covered e/μ-mixing with > GeV covered MAGIC: 158 hr of Segue 1 Fermi-LAT: 6 yr of 15 dsph (incl. Segue 1) DM profile: NFW Fermi-LAT dominates MAGIC in almost all E-range. CTA prospect : 500hr of Milky Way DM profile: Einasto No syst. unc. (stat only) 48 /70

49 Summary σ - ( / ) σ - ( / ) e-mixing μ-mixing τ-mixing CTA 500hr covers > GeV full coverage HL-LHC (slepton) covers < 400 (480) GeV (but not degenerate region) HL-LHC (lepton) covers equivalent to < 350 (430) GeV < 380 (480) GeV e/μ-mixing, QUE ~ ( ) τ/μ-mixing, QUE ~ ( ) τ + τ - - ( ) ( ) 49 /70

50 O u t l i n e Abdullah, Feng, SI, Lillard [ ] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 50 /70

51 MSSM4G : Working assumption (the minimal setup) MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra interaction mh assumed to be equal-mass QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT assumed to be equal-mass extra coupling mh slightly assumed to be equal-mass 51 /70

52 MSSM4G : Working assumption (the minimal setup) MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra lepton search extra QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT slepton search interaction mh assumed to be equal-mass assumed to be equal-mass extra coupling mh slightly assumed to be equal-mass 52 /70

53 MSSM4G : Working assumption (the minimal setup) MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra lepton search extra QDEE (as discussed model before) : MSSM + standard MSSM searches + for vectorlike SU(5) GUT leptons (but 2x in QDEE) gauge coupling unification extra interaction mh assumed to be equal-mass coupling mh slightly slepton search assumed to be equal-mass assumed to be equal-mass 53 /70

54 Collider prospects for extra slepton searches e/μ-mixing slepton searches determined by mixing parameters 14 TeV prospects studied in (Eckel, Ramsey-Musolf, Shepherd, Su) re-interpreted ATLAS (8TeV full) [ ] CMS (8TeV full) [ ] 54 /70

55 Collider prospects for extra slepton searches e/μ-mixing slepton searches determined by mixing parameters 14TeV 0.3, 1, 3/ab 8TeV full 2 lepton + MET + mt2 + jet-veto BKG taken from MG5 Pythia Delphes (also for signal) rescaled by NLO K-factor di-boson dominates Signal events at LO level Uncertainties = stat. + 5% syst. 55 /70

56 Collider prospects for extra slepton searches τ-mixing stau searches determined by mixing parameters No constraint expected. LHC Run 1 provided no limit on MSSM stau mass. 14TeV, 3/ab LHC will not exclude MSSM4G parameter region. 56 /70

57 σ - ( / ) Summary σ - ( / ) e-mixing μ-mixing τ-mixing CTA 500hr covers > GeV full coverage HL-LHC (slepton) covers < 400 (480) GeV (but not degenerate region) HL-LHC (lepton) covers equivalent to < 350 (430) GeV < 380 (480) GeV e/μ-mixing τ/μ-mixing, QUE ~ ( ) ~ ( ) τ + τ - - ( ) ( ) 57 /70

58 Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton searches by multi- signature (3 5 ) [Cf. ATLAS collaboration, ] Monte Carlo simulation 58 /70

59 cross section [fb] Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton 14 TeV LHC searches exclusion exp σ UL;95% byat 300fb 2 e-mixed VLL exp σ at 1000fb 10 multi- signature (3 5 UL;95% exp ) 10 σ UL;95% at 3000fb [Cf. ATLAS collaboration, LO cross ] section (QUE) LO cross section (QDEE) VLL mass [GeV] Snowmass BKG set is used. MG5 Pythia Delphes + NLO K-factor di-boson + tt dominated Signal by FR MG5aMC Pythia Delphes (LO) 0.3/ab 1/ab 3/ab (with 1&2σ band) 14TeV, 3/ab covers < 350 (425) GeV QUE QDEE SR dedicated for WZ / ZZ + leptons 3L, 4L for WZ, and 4L, 5L for ZZ tau-tag / b-tag not used (avoided) Uncertainties = stat. + 20% syst. 59 /70

60 Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton searches by multi- signature (3 5 ) [Cf. ATLAS collaboration, ] τ-mixing case (Kumar and Matrin) SRs: 4(e, mu, had-tau) Signal and BKG by their MC (FR MG5 Pythia Delphes) no prospects for exclusion if BKG syst. unc. > 10% 14TeV, 3/ab covers < 350 (425) GeV QUE QDEE 13 TeV, 3/ab covers < 234 (264) GeV with a very optimistic BKG estimation 60 /70

61 Collider prospects summary e/μ-mixing cases - QUE - QDEE ~ [ ] l ( ) ~ [ ] l ( ) ~ [ ] l ~ [ ] l τ-mixing case LHC insensitive ( ω `) 61 /70

62 Collider Gamma-ray search combination e/μ-mixing cases - QUE - QDEE ~ [ ] l ( ) CTA ~ [ ] l ( ) CTA ~ [ ] l ~ [ ] l τ-mixing case LHC insensitive, but CTA covers full region 62 /70

63 Summary : MSSM4G scenario extra annihilation channel larger proper if Edsjö, Schelke, Ullio, Gondolo, hep-ph/ /70

64 Summary : Future prospects e-mixing μ-mixing τ-mixing CTA 500hr covers > GeV full coverage HL-LHC (slepton) σ - ( / ) covers < 400 (480) GeV (but not degenerate region) HL-LHC (lepton) covers equivalent to < 350 (430) GeV < 380 (480) GeV e/μ-mixing, QUE / QDEE τ/μ-mixing, QUE - - ~ ( ) τ + τ - ~ [ ] l ( ) CTA excl. ~ [ ] l ( ) CTA excl. LHC excl. LHC excl. ( ) ~ [ ] l ~ [ ] l 64 /70

65 O u t l i n e Abdullah, Feng, SI, Lillard [ ] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds : muon g 2 problem 65 /70

66 Muon g-2 Problem anomaly Hagiwara, Liao, Martin, Nomura, Teubner [ ] MSSM: extra contribution MSSM may explain this anomaly. 66 /70

67 Muon g-2 Problem anomaly PUSH UP Hagiwara, Liao, Martin, Nomura, Teubner [ ] MSSM: extra contribution MSSM may explain this anomaly. 4G extra contribution? mixing 67 /70

68 Muon g-2 Problem anomaly PUSH DOWN Hagiwara, Liao, Martin, Nomura, Teubner [ ] MSSM: extra contribution MSSM may explain this anomaly. 4G extra contribution? mixing 68 /70

69 Muon g-2 Problem Why always negative? 69 /70

70 Summary : Future prospects e-mixing μ-mixing τ-mixing CTA 500hr covers > GeV full coverage HL-LHC (slepton) σ - ( / ) covers < 400 (480) GeV (but not degenerate region) HL-LHC (lepton) covers equivalent to < 350 (430) GeV < 380 (480) GeV e/μ-mixing, QUE / QDEE τ/μ-mixing, QUE - - ~ ( ) τ + τ - ~ [ ] l ( ) CTA excl. ~ [ ] l ( ) CTA excl. LHC excl. LHC excl. ( ) ~ [ ] l ~ [ ] l 70 /70