Abstract
We perform an analysis of the simplified dark matter models in the light of cosmic ray observables by AMS-02 and Fermi-LAT. We assume fermion, scalar or vector dark matter particle with a leptophobic spin-0 mediator that couples only to Standard Model quarks and dark matter via scalar and/or pseudo-scalar bilinear. The propagation and injection parameters of cosmic rays are determined by the observed fluxes of nuclei from AMS-02. We find that the AMS-02 observations are consistent with the dark matter framework within the uncertainties. The AMS-02 antiproton data prefer 30 (50) GeV - 5 TeV dark matter mass and require an effective annihilation cross section in the region of 4 × 10−27 (7 × 10−27) - 4 × 10−24 cm3/s for the simplified fermion (scalar and vector) dark matter models. The cross sections below 2 × 10−26 cm3/s can evade the constraint from Fermi-LAT dwarf galaxies for about 100 GeV dark matter mass.
Highlights
Which produces antiproton, in the light of the antiproton flux data newly reported by AMS-02 [9]
If the annihilation cross section calculated by a certain set of mDM and the mediator mass is greater than the upper limit, we claim the corresponding set of mDM, mMed is excluded by Fermi-Large Area Telescope (LAT) dwarf spheroidal satellite galaxies (dSphs)
In this work we investigate the simplified dark matter models favored by the recent AMS02 antiproton data and consider the constraint from no gamma ray excess in Milky Way dSphs
Summary
We describe the considered simplified dark matter models in table 1. Under the above assumptions the dark matter models are described by two parameters, i.e. the dark matter mass mDM = mχ, mφ, mX and the mediator mass mMed = mS2, mS4, mSC or mSV We scan these parameters in the following range. The two types of spectrum are both the annihilation-fraction-weighted sum of the differential yields into specific final states. For. different quark or gluon final states in 2-body spectrum we use PPPC4DMID [28] to generate the differential yield which is weighted by the corresponding annihilation fraction, i.e. σannv qq/ σannv and σannv gg/ σannv. The 4-body cosmic ray spectrum is given by the spectrum of the mediator decay in its rest frame followed by a Lorentz boost [12, 29]. The expressions of mediator decay widths and dark matter annihilation cross sections are collected in appendix
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