Boosted Dark Matter in IceCube and at the Galactic Center

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1 Boosted Dark Matter in IceCube and at the Galactic Center (based on JHEP 1504, 105 (2015) [arxiv: ] ) collaborated with Joachim Kopp, Xiao-ping Wang Jia Liu MITP, Johannes Gutenberg University Mainz TAUP 2015 September, Torino Jia Liu (JGU Mainz) September, / 19

2 IceCube: neutrino track event Credit: IceCube Collaboration muons from charge current interaction Charged Current: ν µ / ν µ + N µ /µ + + N Jia Liu (JGU Mainz) September, / 19

3 IceCube: neutrino shower event Credit: IceCube Collaboration Neutral Current: ν l / ν l + N ν l / ν l + N Charged Current: ν e,τ / ν e,τ + N (e, τ )/(e +, τ + ) + N Jia Liu (JGU Mainz) September, / 19

4 IceCube: highest energy neutrino in history π / all-sky Neutrino Effective Area [m 2 ] ν e ν µ Neutrino Energy [TeV] ν τ Science 342, (2013) Glashow resonance in ν e flavor: e + ν e W roughly same effective area for each flavor at high energy Jia Liu (JGU Mainz) September, / 19

5 IceCube: highest energy neutrino in history Events per 988 Days Background Atmospheric Muon Flux Bkg. Atmospheric Neutrinos (π/k) Background Uncertainties Atmospheric Neutrinos (90% CL Charm Limit) Bkg.+Signal Best-Fit Astrophysical (best-fit slope E 2.3 ) Bkg.+Signal Best-Fit Astrophysical (fixed slope E 2 ) Data Deposited EM-Equivalent Energy in Detector (TeV) neutrino source: p + p π, K µ + ν µ e + 2ν µ + 1ν e π, K source leads flavor ratio (1 : 1 : 1) at Earth best fit flavor (0 : 0.2 : 0.8) ; γ 2.5 (from ) Jia Liu (JGU Mainz) September, / 19

6 IceCube neutrino: possible interpretations Astrophysical neutrinos with spectrum E 2.5 Neutrino from dark matter (energy cutoff) Decaying dark matter Annihilating dark matter ultra-massive long-lived particle Non-standard neutrino interaction (e.g. absorption from resonance) Track event and shower event ratio problem A shower event preferred model? A DM induced collision? (Bhattacharya et al) Jia Liu (JGU Mainz) September, / 19

7 IceCube: track event and shower event ratio π / all-sky Neutrino Effective Area [m 2 ] ν e ν µ Neutrino Energy [TeV] Mild lack of ν µ neutrino suggested by C.-Y. Chen, P. Bhupal Dev, and A. Soni; O. Mena, S. Palomares-Ruiz, and A. C. Vincent However, The event (J2000.0) multi-pev neutrino-induced muon event a total energy of 2.6 ± 0.3 PeV within the instrumented volume of IceCube Need astrophysical component or DM-induced charged current (e.g. sneutrino DM) ν τ Jia Liu (JGU Mainz) September, / 19

8 Summary of motivations IceCube a model with shower events preference at high energy Fermi-LAT gamma-ray excess at 2GeV at GC Jia Liu (JGU Mainz) September, / 19

9 Fermi-LAT: Galactic Center Excess Excess of gamma-ray at GC, peak around 2GeV Dark matter annihilation bb, f 2 σv rel b b cm 3 /s Dark matter mass 30GeV 50GeV ( ) Jia Liu (JGU Mainz) September, / 19

10 Model Lagrangians Two dark matter φ, in dark sector has boosted component and thermal component (see also Lina Necib, Monday) L DS 1 2 ( µ φ)( µ φ) 1 2 m2 φ φ2 + i / m y φ φ (1) One pseudoscalar a connect dark sector and SM L int ig a γ 5 + i f g Yf 2mf v a f γ 5 f (2) 6 free parameters m a, m φ, m, y φ, g, g Y Jia Liu (JGU Mainz) September, / 19

11 Model UV complete models MSSM-like model iah 1 H 2 + h.c. leads to pseudoscalar a and A 0 mixing g Yd = g Yl = tan β sin θ/ 2 (3) g Yu = cot β sin θ/ 2 (4) Flipped model iah 1 H 2 + h.c. leads to pseudoscalar a and A 0 mixing g Yd = tan β sin θ/ 2 (5) g Yu = g Yl = cot β sin θ/ 2 (6) Vector-like quark model Integrating out heavy vector-like quark which mixes with SM quark y Ψ a Qγ 5 Ψ + y mix ΨHdR + y Q QHdR dγ 5 d R a (7) Jia Liu (JGU Mainz) September, / 19

12 IceCube spectrum fitting Fitting a q q (Primary signal) DM scattering shower events only φ a (Secondary signal) neutrinos from a decay both shower and track events Primary: φ, scatters with quark Secondary: φ + a, a decays to b quark, producing neutrinos Jia Liu (JGU Mainz) September, / 19

13 Fitting IceCube spectrum fitting m a m φ m g Yb g τ φ /f φ σv rel b b f BR 3(φ a) Comment [GeV] [PeV] [GeV] [10 25 s] [10 26 cm 3 /s] BP Vector-like BP m =30GeV,m a=12gev,m ϕ=4.5pev 100 g 2 f ϕ/τ ϕ= s -1 (g g Yb ) 2 f ϕ/τ ϕ= s IceCube Total ATM Neutrino DM-EG DM-GC 500 m =30GeV,m a=80gev,m ϕ=3.9pev 100 g 2 f ϕ/τ ϕ= s -1 (g g Yb ) 2 f ϕ/τ ϕ= s IceCube Total ATM Neutrino DM-EG DM-GC [ ] [ ] (BP 1) (BP 2) Jia Liu (JGU Mainz) September, / 19

14 IceCube spectrum fitting ( LLR m φ, gy 2 g 2 b f φ, g 2 f ) Max φ x [, ] = log τ φ τ φ Fitting [ f Gauss (x) ( i f Poisson (S i m φ, g 2 Y b g 2 f φ, g2 f ) φ τ φ τ φ [ Max x f Gauss (x ) i f ( Poisson Bi + x ) ] B Oi i [, ] )] + B i + x B i Oi ϕ /τϕ [ - - ] dof Benchmark +Bestfit 3σ 2σ 1σ + + 1σ m =30GeV m a=80gev m a=12gev diffuse γ (m a=80gev) diffuse γ (m a=12gev) 3σ 2σ ϕ /τϕ [ - - ] m =30GeV m a=80gev m a=12gev 3σ 2σ 1σ + 3σ 2σ 1σ + 2dof Benchmark +Bestfit ( ) ϕ /τϕ [ - - ] dof Benchmark +Bestfit + 1σ + 1σ 2σ 2σ m =30GeV m a=80gev m a=12gev 3σ 3σ ϕ [ ] ( ) ϕ /τϕ [ - - ] ϕ [ ] 6 free parameters m a, m φ, m, y φ, g, g Y m fixed by Fermi-LAT, m a chose by hand = 1 free parameter fixed by relic density and Fermi-LAT. Jia Liu (JGU Mainz) September, / 19

15 Fitting DM relic density Relic density Non-thermal production mechanism for PeV φ Thermal production for 30 GeV f φ + f = 1 and f,φ Ω,φ /Ω DM f a annihilation channels a f a m a m φ m g Yb g τ φ /f φ σv rel b b f BR 3(φ a) Comment [GeV] [PeV] [GeV] [10 25 s] [10 26 cm 3 /s] BP Vector-like BP Fermi-LAT requirement satisfied f 2 σv rel b b cm 3 /s Jia Liu (JGU Mainz) September, / 19

16 Constraints Electron and positron constraint φ a a bb produce secondary ν, e and γ ϕ ± / [ ] m ϕ =4.5PeV,m =30GeV,m a =12GeV Fermie + +e - H.E.S.S.e + +e - ϕ a g 2 f ϕ /τ ϕ ~ s -1 AMS-02e + BKGe + SIG+BKGe + BKGe + +e - SIG+BKGe + +e - ϕ ± / [ ] m ϕ =3.9PeV,m =30GeV,m a =80GeV Fermie + +e - H.E.S.S.e + +e - ϕ a g 2 f ϕ /τ ϕ ~ s -1 AMS-02e + BKGe + SIG+BKGe + BKGe + +e - SIG+BKGe + +e [ ] [ ] Jia Liu (JGU Mainz) September, / 19

17 Gamma ray constraint Constraints φ a a bb produce secondary ν, e and γ γ ϕ/ γ [ ] m =30GeV,m a =12GeV m ϕ =4.5PeV ϕ a,a bb ϕ/τϕ ~ γ [ ] γ ϕ/ γ [ ] m =30GeV,m a =80GeV m ϕ =3.9PeV ϕ a,a bb ϕ/τϕ ~ γ [ ] Jia Liu (JGU Mainz) September, / 19

18 Constraints Other constraints Direct detection constraint Flavor physics, e.g. B s µ + µ Collider constraint, e.g. h aa and heavy quark limits IceCube galactic center e ± diffuse γ Lab Boosted DM Secondary ν m a m φ gy 2 g 2 b f φ/τ φ g 2 f φ/τ φ m σv rel b b f 2 g 2 f φ/τ φ g 2 f φ/τ φ Model g Yb [GeV] [PeV] [10 26 s 1 ] [10 26 s 1 ][GeV] [10 26 cm 3 /s] [10 26 s 1 ] [10 26 s 1 ] MSSM-like Flipped tan β Vector-quark 20 MSSM-like Flipped Vector-quark 20 Jia Liu (JGU Mainz) September, / 19

19 Conclusion Summary 500 m =30GeV,m a=80gev,m ϕ=3.9pev 100 g 2 f ϕ/τ ϕ= s -1 (g g Yb ) 2 f ϕ/τ ϕ= s IceCube Total ATM Neutrino DM-EG DM-GC [ ] IceCube a peaked shower event contribution ( neutral current scattering) Fermi-LAT gamma-ray excess at 2GeV at GC ( bb) (J2000.0) event calls for astrophysical component or DM with charged current interaction (e.g. sneutrino DM) Jia Liu (JGU Mainz) September, / 19