Testing dark sectors with vector mediators using ANTARES and IceCube search data for neutrino lines from dark matter annihilation in the galactic halo

Van Thi Dieu Hien and G.-L. Lin Testing dark sectors with vector mediators using ANTARES and IceCube search data for neutrino lines from dark matter annihilation in the galactic halo XXI International Workshop on Neutrino Telescopes at Padova, Italy DIFFERENT APPROACHES FOR PROBING DARK MATTER Sun Galactic Halo ANTARES/KM3NeT and IceCube search 101102103104105 mχ[GeV] 10−26 10−25 10−24 10−23 10−22 10−21 ⟨σv⟩[cm3s−1] IceCube Tracks χ¯χ→ν¯ν, NFW ANTARES Tracks + air showers χ¯χ→ν¯ν, NFW Dirac χ, upper limits at 90% C.L. R. Abbasi, et al., Phys. Rev. D 108, 102004 (2023) S. R. Gozzini on behalf of the ANTARES and KM3NeT Collaborations, J. Instrum. 16 (2021) C09006. **Factor of two multiplied for Dirac DM TWO QUESTIONS TO CONSIDER: Are there models with a significant branching fraction of DM annihilating to neutrinos? Could at the present universe enhance over its value at thermal freeze-out? ⟨σv⟩ MODELS FAVORING χ¯χ→ν¯ν Dark bosons with mass mixing with Standard Model Z boson Kinetic mixing Mass mixing mV≪mZ G.-L. Lin and Y.-H. Lin, Phys. Rev. D 104 (2021) 063021 MODELS FAVORING χ¯χ→ν¯ν Extension of model with vector boson coupling to fermionic dark matter U(1)Lμ−Lτ Qαβ = diag(0,1, −1) ℒχ=−1 4Z′ μνZ′ μν −1 2m2 Z′ Z′ μZ′ μ−mχ¯χχ +gχZ′ μ¯χγμχ +gZ′ Z′ μQαβ(¯ lαγμlβ+ ¯ναγμPLνβ) Z’ decays to neutrinos with high branching ratios 1. X.-G. He, G. C. Joshi, H. Lew, and R. R. Volkas, Phys. Rev. D 44, 2118 (1991). 2. J. H. Chang, R. Essig, and S. D. McDermott, J. High Energy Phys. 09 (2018) 051. 3. P. Foldenauer, Phys. Rev. D 99, 035007 (2019). 4. M. Escudero, D. Hooper, G. Krnjaic, and M. Pierre, J. High Energy Phys. 03 (2019) 071. 5.D. Croon, G. Elor, R. K. Leane, and S. D. McDermott, J. High Energy Phys. 01 (2021) 107. We take the DM extension of model for subsequent discussions. The results can be applied to other models with corrections in decay branching ratios to neutrinos. U(1)Lμ−Lτ THE VALUE OF FOR PRODUCING THERMAL RELIC ABUNDANCE ⟨σv⟩ ΩCDMh2 at the thermal freeze-out as a function of ⟨σv⟩ mχ dn dt + 3Hn =⟨σv⟩(n2 eq −n2) values for producing correct relic abundance ⟨σv⟩ G. Steigman, B. Dasgupta and J. F. Beacom, Phys. Rev. D 86 (2012) 023506 ENHANCEMENT OF AT THE PRESENT UNIVERSE OVER ITS VALUE AT THERMAL FREEZE-OUT—RESONANT MECHANISM ⟨σv⟩ ⟨σvrel⟩=1 (2πv2 0)3∫dv1dv2e−(v2 1+v2 2)/2v2 02σβi vrel =v1− v2= 2βi βi= 1 −4m2 χ/E2 cm The S-channel annihilation process χχ →M→f¯ f M. Ibe, H. Murayama and T. T. Yanagida, Phys. Rev. D 79 (2009) 095009 • slightly larger than for enhancement. •However, suppression occurs if is smaller than . 2mχ M 2mχ M •Both solutions yield the correct relic abundance. •In some cases, no solution exists or both solutions occur at , i.e., . mZ′ > 2mχ δχ< 0 gχ=gZ′ = 10−2 And these white region here show no solution produced by thermal relic in the ealy 101102103104105 mχ[GeV] 10−31 10−29 10−27 10−25 10−23 10−21 10−19 ⟨σv⟩[cm3s−1] gχ=g Z′=10−2 101102103104105 mχ[GeV] 10−30 10−28 10−26 10−24 10−22 10−20 ⟨σv⟩[cm3s−1] gχ=g Z′=10−1 gχ=gZ′ = 10−1 δχ< 0 δχ< 0 δχ> 0 101102103104105 mχ[GeV] 10−33 10−31 10−29 10−27 10−25 10−23 10−21 10−19 ⟨σv⟩[cm3s−1] gχ=g Z′=10−3 gχ=gZ′ = 10−3 •As constraints on the couplings become more stringent, the parameter space that supports the thermal freeze-out scenario shrinks further. •For large coupling constants ( ), thermal freeze-out works for and the prediction remains consistent with the data. gχ=gZ′ = 10−1 102<mχ/GeV < 104 mχ>mZ′ The annihilation process through Z′ :χ¯χ→Z′ Z′ →ν¯νν¯ν is determined by the relic abundance (summing and ). → αχ Ωh2= 0.12 χ ¯χ . S=1 The relic abundance of is then given by χ, ¯χ Ωh2=2(1.07 ×109) GeV−1 Jg1/2 *Mpl . xf=ln 0.152 Mpl mχ⟨σv⟩ g1/2 *x1/2 f . Mpl = 1.22 ×1019GeV, J=∫∞ xf ⟨σv⟩ x2dx , Three mass ratios considered: mZ′ /mχ= 0.1, 0.01, and 0.001. ⟨σv⟩early =1 8m4 χTK2 2(mχ/T)∫∞ 4m2 χ ds σ(s)s(s−4m2 χ)K1(s T)S S=2παχ/vrel 1−e−2παχ/vrel ;αχ=g2 χ 4π In the early universe: the DM relative velocity is high, vrel →S≈1 Jonathan L. Feng, Manoj Kaplinghat, and Hai-Bo Yu, PRL 104, 151301 (2010) Here S is the Sommerfeld factor. K. Griest, D. Seckel, Phys. Rev. D 43 (1991) 3191–3203 P. Gondolo, G. Gelmini, Nucl. Phys. B 360 (1) (1991) 145–179 mZ′ mχ =6αχ π2n2,n= 1,2,... mZ′ = 0.1mχ 102103104 mχ[GeV] 10−5 10−4 10−3 10−2 10−1 100 101 102 αχ αχand Ωχh2=0.12 mZ′=0.1mχ,χ¯χ→Z′Z′→ν¯νν¯ν 102103104 mχ[GeV] 10−5 10−4 10−3 10−2 10−1 100 101 102 αχ n=1 n=2 n=3 αχand Ωh2=0.12 mZ′=0.1mχ The resonance enhancement occurs at 2 points, which happens when mχ= 4650 GeV mχ= 18021 GeV S. Tulin, H. B. Yu, and M. Zurek, Phys. Rev. D 87, 115007 More DM mass points are taken in the vicinity of resonance The phenomenological study by B. Dasgupta and R. Laha, Phys. Rev. D 86,093001 (2012) shows that IceCube/KM3NeT sensitivities to differ from their sensitivities to only within a factor of 2 if decays exclusively to . ⟨σ(χ¯χ→ν¯ν)v⟩ ⟨σ(χ¯χ→Z′ Z′ →ν¯νν¯ν)v⟩ Z′ ν¯ν Comparison for track event spectra resulting from muon neutrinos in and χ¯χ→ν¯ν χ¯χ→Z′ Z′ →ν¯νν¯ν 102103104105 mχ[GeV] 10−27 10−26 10−25 10−24 10−23 10−22 10−21 10−20 10−19 ⟨σv⟩[cm3s−1] IceCube Tracks 90% C.L. ANTARES Tracks + air showers 90% C.L. Early universe Present-day universe w/ S mZ′=0.1mχ,χ¯χ→Z′Z′→ν¯νν¯ν Taken as sensitivities to χ¯χ→Z′ Z′ →ν¯νν¯ν 102103104105 mχ[GeV] 10−27 10−26 10−25 10−24 10−23 10−22 10−21 10−20 10−19 ⟨σv⟩[cm3s−1] IceCube Tracks 90% C.L. ANTARES Tracks + air showers 90% C.L. Early universe Present-day universe w/ S mZ′=0.01mχ,χ¯χ→Z′Z′→ν¯νν¯ν 102103104105 mχ[GeV] 10−27 10−26 10−25 10−24 10−23 10−22 10−21 10−20 10−19 ⟨σv⟩[cm3s−1] IceCube Tracks 90% C.L. ANTARES Tracks + air showers 90% C.L. Early universe Present-day universe w/ S mZ′=0.001mχ,χ¯χ→Z′Z′→ν¯νν¯ν For a smaller ratio, Sommerfeld enhancement begins to take effect at the smaller . mZ′ /mχ mχ