MSSM scenario Sho IWAMOTO 25 Dec. 2016 IPS 62nd annual meeting @ TelAviv University Based on [1608.00283] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine)
The Standard Model of Particle Physics hepex topics of this room hepph hepth 2 /39
The Standard Model of Particle Physics hepex topics of this room my research field hepph hepth 3 /39
The Standard Model of Particle Physics hepex this work topics of this room my research field hepph hepth 4 /39
The Standard Model of Particle Physics hepex this work topics of this room my research field hepph hepth 5 /39
Physics beyond the Standard Model Problems of the Standard Model = Hints of New Physics Anomalies in Bphysics Proton charge radius Beryllium anomaly Muon g 2 Higgs mass ( naturalness ) Neutrino mass Dark matter Unification of 3 forces Dark energy Gravity 6 /39
Physics beyond the Standard Model New Physics Candidates SUSY [supersymmetry] etc Please fill this list with your models / models you like Problems of the Standard Model = Hints of New Physics Anomalies in Bphysics Proton charge radius Beryllium anomaly Muon g 2 Higgs mass ( naturalness ) Neutrino mass Dark matter Unification of 3 forces Dark energy Gravity 7 /39
Physics beyond the Standard Model New Physics Candidates SUSY etc Problems of the Standard Model = Hints of New Physics Anomalies in Bphysics Proton charge radius Beryllium anomaly Muon g 2 Higgs mass ( naturalness ) Neutrino mass Dark matter Unification of 3 forces Dark energy Gravity 8 /39
Physics beyond the Standard Model New Physics Candidates SUSY etc Problems of the Standard Model = Hints of New Physics Anomalies in Bphysics Proton charge radius Beryllium anomaly Muon g 2 Higgs mass ( naturalness ) Neutrino mass Dark matter Unification of 3 forces Dark energy Gravity 9 /39
Physics beyond the Standard Model New Physics Candidates SUSY etc Problems of the Standard Model = Hints of New Physics Anomalies in Bphysics Proton charge radius Beryllium anomaly Muon g 2 Higgs mass ( naturalness ) Neutrino mass Dark matter Unification of 3 forces Dark energy Gravity 10 /39
Dark matter candidate in MSSM MSSM Dark matter candidate SUSY Higgs SM 11 /39
Dark matter candidate in MSSM MSSM Dark matter candidate Pure dark matter (i.e., DM is and it is purely like) theoretically motivated & simple thermal overabundance problem MSSM4G model as one solution 12 /39
O U T L I N E Abdullah, Feng, SI, Lillard [1608.00283] Introduction: Overabundant problem Model: MSSM Phenomenology: Gammaray obs. & LHC Summary 13 /39
Bino relic density Early Universe with pair creation equilibrium pair annihilation 14 /39
Bino relic density Early Universe with pair creation equilibrium pair annihilation 15 /39
Bino relic density Early Universe with pair creation pair annihilation relic density far apart due to pair annihilation Universe s expansion 16 /39
Bino relic density Early Universe with pair creation pair annihilation relic density far apart due to pair annihilation Universe s expansion Figure from Gelmini and Gondolo, 1009.3690 17 /39
Bino relic density pure DM 100 GeV: DM density ( relic density ) ~ observation 100 GeV: smaller crosssection larger DM density overabundant problem of Bino thermal relic DM Figure from Gelmini and Gondolo, 1009.3690 18 /39
Bino relic density pure DM 100 GeV: DM density ( relic density ) ~ observation 100 GeV: smaller crosssection larger DM density DM is not pure? pure DM overabundant problem of Bino thermal relic DM mixing Other annihilation channels? coannihilation [Griest, Seckel, 1991] MSSM4G [Abdullah, Feng, 2015] 19 /39
O U T L I N E Abdullah, Feng, SI, Lillard [1608.00283] Introduction: Overabundant problem Model: MSSM Phenomenology: Gammaray obs. & LHC Summary 20 /39
MSSM4G outline Image by MissBJ [CC BY 3.0], via Wikimedia Commons SM = 3Generations MSSM = 3Generations SUSY extra vectorlike 4 th Generation lepton MSSM4G 21 /39
MSSM4G outline A new solution to overabundant problem: MSSM4G extra annihilation channel if 22 /39
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 23 /39
MSSM4G : Two models QUE model QDEE model Abdullah, Feng [1510.06089] color bands show 24 /39
O U T L I N E Abdullah, Feng, SI, Lillard [1608.00283] Introduction: Overabundant problem Model: MSSM Phenomenology: Gammaray obs. & LHC Summary 25 /39
Constraints from cosmicray observations DM indirect detection by Gammaray observation DM DM ~ 2 : 1 : 1 26 /39
Constraints from cosmicray observations DM indirect detection by Gammaray observation DM DM FermiLAT (satellite) MAGIC (Air Cherenkov telescope) CTA (future A. C. Telescope) 27 /39
σ ( / ) Gammaray searches in QUE models ~ ( ) Abdullah, Feng, SI, Lillard [1608.00283] valid for any mixing patterns + MSSM4G region MAGIC: 158 hr of Segue 1 FermiLAT: 6 yr of 15 dsph (incl. Segue 1) DM profile: NFW FermiLAT dominates MAGIC in almost all Erange. ( ) CTA prospect : 500hr of Milky Way DM profile: Einasto No syst. unc. (stat only) 28 /39
σ ( / ) Gammaray searches in QUE models Abdullah, Feng, SI, Lillard [1608.00283] if 4G lepton decays to taulepton ~ ( ) τ + τ MSSM4G region future sensitivity MAGIC: 158 hr of Segue 1 FermiLAT: 6 yr of 15 dsph (incl. Segue 1) DM profile: NFW FermiLAT dominates MAGIC in almost all Erange. ( ) CTA prospect : 500hr of Milky Way DM profile: Einasto No syst. unc. (stat only) 29 /39
O U T L I N E Abdullah, Feng, SI, Lillard [1608.00283] Introduction: Overabundant problem Model: MSSM Phenomenology: Gammaray obs. & LHC Summary 30 /39
LHC prospects (4G slepton) search (4G lepton) search * searches for 2lepton + Missing E T searches for multilepton final state (same as MSSM slepton searches) 31 /39
Collider prospects summary if 4G lepton decays to electron or muon QUE QDEE ~ [ ] l ( ) ~ [ ] l ( ) ~ [ ] l ~ [ ] l if 4G lepton decays to taulepton LHC insensitive ( ω `) 32 /39
Collider Gammaray search combination if 4G lepton decays to electron or muon QUE QDEE ~ [ ] l ( ) CTA ~ [ ] l ( ) CTA ~ [ ] l ~ [ ] l if 4G lepton decays to taulepton LHC insensitive ( ω `) 33 /39
O U T L I N E Abdullah, Feng, SI, Lillard [1608.00283] Introduction: Overabundant problem Model: MSSM Phenomenology: Gammaray obs. & LHC Summary 34 /39
Summary σ ( / ) Pure DM with may cause 100 GeV DM overabundance MSSM4G: is provides a solution additional to this problem. DMannihilation channel. correct relic density even w. 100 GeV. MSSM4G will be covered ALL explored by CTA soon. & HLLHC: if 4G lepton decays to electron or muon taulepton ~ ( ) τ + τ ~ [ ] l ( ) covered by CTA All covered by CTA covered by HLLHC ~ [ ] l ( ) 35 /39
Summary σ ( / ) Pure DM with 100 GeV DM overabundance MSSM4G: is provides a solution additional to this problem. DMannihilation channel. correct relic density even w. 100 GeV. MSSM4G will be covered ALL explored by CTA soon. & HLLHC: if 4G lepton decays to electron or muon taulepton ~ ( ) τ + τ ~ [ ] l ( ) covered by CTA All covered by CTA covered by HLLHC ~ [ ] l ( ) 36 /39
Summary σ ( / ) Pure DM with 100 GeV DM overabundance MSSM4G: provides additional DMannihilation channel. correct relic density even w. 100 GeV. MSSM4G will be covered ALL explored by CTA soon. & HLLHC: if 4G lepton decays to electron or muon taulepton ~ ( ) τ + τ ~ [ ] l ( ) covered by CTA covered by HLLHC All covered by CTA ~ [ ] l ( ) 37 /39
Summary σ ( / ) Pure DM with 100 GeV DM overabundance MSSM4G: provides additional DMannihilation channel. correct relic density even w. 100 GeV. MSSM4G will be covered by CTA & HLLHC: if 4G lepton decays to electron or muon taulepton ~ ( ) τ + τ ~ [ ] l ( ) covered by CTA covered by HLLHC All covered by CTA ~ [ ] l ( ) 38 /39
Summary σ ( / ) Pure DM with 100 GeV DM overabundance MSSM4G: provides additional DMannihilation channel. correct relic density even w. 100 GeV. MSSM4G will be covered by CTA & HLLHC: if 4G lepton decays to electron or muon taulepton ~ ( ) τ + τ ~ [ ] l ( ) covered by CTA covered by HLLHC All covered by CTA ~ [ ] l ( ) 39 /39