MSSM scenario Sho IWAMOTO 15 Sep. 2016 Seminar @ Osaka University Based on [1608.00283] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine)
The Standard Model of Particle Physics Universe = Image by MissBJ [CC BY 3.0], via Wikimedia Commons 2 /72
The Standard Model of Particle Physics Universe = dark matter? 3 /72
The Standard Model of Particle Physics Universe = dark energy? dark matter? 4 /72
Physics beyond the Standard Model Hints of New Physics Dark matter Dark energy Neutrino mass Gauge coupling unification Higgs mass ( naturalness ) Muon... 5 /72
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 /72
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 /72
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 /72
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 /72
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... 10 /72
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 /72
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 /72
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... 13 /72
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... 14 /72
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/9709356 15 /72
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/9709356 16 /72
Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least 1010 yr) charge neutral density not detected by astrophysics / direct search / LHC 17 /72
Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least 1010 yr) charge neutral density not detected by astrophysics / direct search / LHC 18 /72
Dark matter candidate in MSSM MSSM Dark matter candidate Dark matter? stable (at least 1010 yr) charge neutral density not detected by astrophysics / direct search / LHC 19 /72
Neutralino relic density overabundant problem 20 /72
Neutralino relic density overabundant problem MSSM model solves this problem! 21 /72
O u t l i n e Abdullah, Feng, SI, Lillard [1608.00283] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 22 /72
Bino relic density Early Universe with pair creation equilibrium pair annihilation 23 /72
Bino relic density Early Universe with pair creation equilibrium pair annihilation 24 /72
Bino relic density Early Universe with pair creation pair annihilation far apart due to pair annihilation Universe s expansion relic density 25 /72
Bino relic density observed relic density proper crosssection of (DM)(DM) SM Figure from Gelmini and Gondolo, 1009.3690 26 /72
Bino relic density observed relic density proper crosssection of (DM)(DM) SM pure -DM (i.e., LSP is -like) strongly depends on 27 /72
Bino relic density observed An example relic density in CMSSM: proper crosssection of (DM)(DM) SM pure -DM (i.e., LSP is -like) strongly depends on Figure from Edsjö, Schelke, Ullio, Gondolo, hep-ph/0301106 28 /72
Co-annihilation An old solution to increase : co-annihilation mass splitting 29 /72
Co-annihilation An old An solution example to increase CMSSM: : co-annihilation mass splitting Figure from Edsjö, Schelke, Ullio, Gondolo, hep-ph/0301106 30 /72
Co-annihilation An old An solution example to increase CMSSM with : co-annihilation -coann.: mass splitting Figure from Edsjö, Schelke, Ullio, Gondolo, hep-ph/0301106 31 /72
O u t l i n e Abdullah, Feng, SI, Lillard [1608.00283] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 32 /72
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) 33 /72
MSSM4G outline A new solution to increase : MSSM4G extra annihilation channel larger proper if 34 /72
MSSM4G outline [MSSM] [MSSM4G] [vector-like mass] [mixing with SM leptons] 35 /72
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 36 /72
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 37 /72
MSSM4G : Working assumption (the minimal setup) MSSM + QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra breaks coupling unification interaction mh QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra 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. 38 /72
MSSM4G : Working assumption (the minimal setup) MSSM + QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra breaks coupling unification interaction mh QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra coupling mh slightly Other working assumptions assumed to be equal-mass assumed to be equal-mass LSP is -like All the other SUSY particles & extra Higgses are decoupled. assumed to be equal-mass 39 /72
MSSM4G : Two models QUE model QDEE model Abdullah, Feng [1510.06089] color bands show 40 /72
MSSM4G : Two models QUE model QDEE model Abdullah, Feng [1510.06089] color bands show vanilla stau-coann. QUE QDEE 41 /72
O u t l i n e Abdullah, Feng, SI, Lillard [1608.00283] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 42 /72
Constraints from cosmic-ray observations DM indirect detection (= searches for DM annihilation) DM DM DM DM time 43 /72
Constraints from cosmic-ray observations DM indirect detection (= searches for DM annihilation) DM DM DM DM time 44 /72
Constraints from cosmic-ray observations DM indirect detection (= searches for ) DM DM [vector-like mass] [mixing with SM leptons] 45 /72
Constraints from cosmic-ray observations DM indirect detection DM DM 46 /72
Constraints from cosmic-ray observations DM indirect detection DM DM insensitive (IceCube) less sensitive / large BKG uncertainty 47 /72
Gamma-ray searches in QUE models ~ ( ) Abdullah, Feng, SI, Lillard [1608.00283] valid for any mixing patterns + - σ - ( / ) 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) 48 /72
Gamma-ray searches in QUE models WW (any mixing pattern) ~ ( ) Abdullah, Feng, SI, Lillard [1608.00283] ττ (only for τ-mixing cases) ~ ( ) + - - τ + τ - σ - ( / ) - σ - ( / ) ( ) ( ) τ-mixing fully covered e/μ-mixing with > 340 380 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) 49 /72
Gamma-ray searches in QDEE models WW (any mixing pattern) ~ ( ) Abdullah, Feng, SI, Lillard [1608.00283] ττ (only for τ-mixing cases) ~ ( ) + - - τ + τ - σ - ( / ) - σ - ( / ) ( ) ( ) τ-mixing fully covered e/μ-mixing with > 340 380 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) 50 /72
Summary e-mixing μ-mixing τ-mixing CTA 500hr covers > 340 380 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 - σ - ( / ) - σ - ( / ) ( ) ( ) 51 /72
O u t l i n e Abdullah, Feng, SI, Lillard [1608.00283] Introduction: why overabundant? Model: MSSM solves overabundance. Analysis: cosmic rays (CTA, Fermi, MAGIC) colliders (LHC) direct detection (LUX) Summary with discussion seeds 52 /72
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 extra coupling mh slightly assumed to be equal-mass assumed to be equal-mass 53 /72
MSSM4G : Working assumption (the minimal setup) MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra lepton search extra interaction mh QDEE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra coupling mh slightly slepton search assumed to be equal-mass assumed to be equal-mass assumed to be equal-mass 54 /72
MSSM4G : Working assumption (the minimal setup) MSSM + breaks coupling unification QUE model : MSSM + gauge coupling unification MSSM + SU(5) GUT extra lepton search extra interaction mh QDEE (as discussed model before) : MSSM + standard MSSM searches + for vectorlike SU(5) GUT leptons (but 2x in QDEE) gauge coupling unification extra coupling mh slightly slepton search assumed to be equal-mass assumed to be equal-mass assumed to be equal-mass 55 /72
Collider prospects for extra slepton searches e/μ-mixing slepton searches determined by mixing parameters 14 TeV prospects studied in 1408.2841 (Eckel, Ramsey-Musolf, Shepherd, Su) re-interpreted ATLAS (8TeV full) [1403.5294] CMS (8TeV full) [1405.7570] 56 /72
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 1408.2841 MG5 Pythia Delphes (also for signal) rescaled by NLO K-factor di-boson dominates Signal events at LO level Uncertainties = stat. + 5% syst. 57 /72
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. 58 /72
Summary e-mixing μ-mixing τ-mixing CTA 500hr covers > 340 380 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 - σ - ( / ) - σ - ( / ) ( ) ( ) 59 /72
Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton searches by multi- signature (3 5 ) [Cf. ATLAS collaboration, 1506.01291] Monte Carlo simulation 60 /72
Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton 14 TeV LHC searches exclusion exp σ UL;95% by at 300fb 2 e-mixed VLL exp σ at 1000fb 10 multi- signature (3 5 UL;95% exp ) cross section [fb] 10 σ UL;95% at 3000fb [Cf. ATLAS collaboration, LO cross 1506.01291] section (QUE) LO cross section (QDEE) 200 250 300 350 400 450 500 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) 0.3ab 1ab 3ab (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. 61 /72
Collider prospects for extra vectorlike lepton searches e/μ-mixing case vectorlike lepton searches by multi- signature (3 5 ) [Cf. ATLAS collaboration, 1506.01291] τ-mixing case 1510.03456 (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 62 /72
Collider prospects summary e/μ-mixing cases - QUE - QDEE - - - - ~ [ ] l ( ) ~ [ ] l ( ) ~ [ ] l ~ [ ] l τ-mixing case LHC insensitive ( ω `) 63 /72
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 64 /72
Summary : MSSM4G scenario extra annihilation channel larger proper if Edsjö, Schelke, Ullio, Gondolo, hep-ph/0301106 65 /72
Summary : Future prospects e-mixing μ-mixing τ-mixing CTA 500hr covers > 340 380 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 / QDEE τ/μ-mixing, QUE - - ~ ( ) - - - - - τ + τ - ~ [ ] l ( ) CTA excl. ~ [ ] l ( ) CTA excl. σ - ( / ) LHC excl. LHC excl. ( ) ~ [ ] l ~ [ ] l 66 /72
O u t l i n e Abdullah, Feng, SI, Lillard [1608.00283] 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 67 /72
Muon g-2 Problem anomaly Hagiwara, Liao, Martin, Nomura, Teubner [1105.1439] MSSM: extra contribution MSSM may explain this anomaly. 68 /72
Muon g-2 Problem anomaly PUSH UP Hagiwara, Liao, Martin, Nomura, Teubner [1105.1439] MSSM: extra contribution MSSM may explain this anomaly. 4G extra contribution? mixing 69 /72
Muon g-2 Problem anomaly PUSH DOWN Hagiwara, Liao, Martin, Nomura, Teubner [1105.1439] MSSM: extra contribution MSSM may explain this anomaly. 4G extra contribution? mixing 70 /72
Muon g-2 Problem Why always negative? 71 /72
Summary : Future prospects e-mixing μ-mixing τ-mixing CTA 500hr covers > 340 380 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 / QDEE τ/μ-mixing, QUE - - ~ ( ) - - - - - τ + τ - ~ [ ] l ( ) CTA excl. ~ [ ] l ( ) CTA excl. σ - ( / ) LHC excl. LHC excl. ( ) ~ [ ] l ~ [ ] l 72 /72