Origins of sharp cosmic-ray electron structures and the DAMPE excess

Abstract

Nearby sources may contribute to cosmic-ray electron (CRE) structures at high energies. Recently, the first DAMPE results on the CRE flux hinted at a narrow excess at energy ∼ 1.4 TeV. We show that in general a spectral structure with a narrow width appears in two scenarios: I) "Spectrum broadening" for the continuous sources with a δ-function-like injection spectrum. In this scenario, a finite width can develop after propagation through the Galaxy, which can reveal the distance of the source. Well-motivated sources include mini-spikes and subhalos formed by dark matter (DM) particles χs which annihilate directly into e + e − pairs. II) "Phase-space shrinking" for burst-like sources with a power-law-like injection spectrum. The spectrum after propagation can shrink at a cooling-related cutoff energy and form a sharp spectral peak. The peak can be more prominent due to the energy-dependent diffusion. In this scenario, the width of the excess constrains both the power index and the distance of the source. Possible such sources are pulsar wind nebulae (PWNe) and supernova remnants (SNRs). We analysis the DAMPE excess and find that the continuous DM sources should be fairly close within ∼ 0.3 kpc, and the annihilation cross sections are close to the thermal value. For the burst-like source, the narrow width of the excess suggests that the injection spectrum must be hard with power index significantly less than two, the distance is within ∼ (3 − 4) kpc, and the age of the source is ∼ 0.16 Myr. In both scenarios, large anisotropies in the CRE flux are predicted. We identify possible candidates of mini-spike and PWN sources in the current Fermi-LAT 3FGL and ATNF catalog, respectively. The diffuse γ-rays from these sources can be well below the Galactic diffuse γ-ray backgrounds and less constrained by the Ferm-LAT data, if they are located at the low Galactic latitude regions.

Bayesian analysis of the break in DAMPE lepton spectra

“…The red cross lines and marks in each plot indicates the best-fit value (largest likelihood). nihilation from a local DM sub-structure [17][18][19][20][21][22][23][123][124][125][126]. Both of these situations call for DM particles with m χ ∼ 1 − 2 TeV.…”

Model-independent analysis of the DAMPE excess

“…The result immediately generated considerable interest [32][33][34][36][37][38][39][40][41][42][43][44][45][46][47][48] and particle dark matter interpretations have already been investigated. In [32] they consider lepton portal, lepton flavour and TeV right-handed neutrino models.…”

TeV dark matter and the DAMPE electron excess

“…In the case where DM annihilates into on-shell X bosons, in order to produce the sharp excess in the energy spectrum, the mass gap between the DM and the X boson has to be in the GeV range. Note added.-After the submission of the first version of our paper on arXiv, a number of papers appeared to interpret the DAMPE anomaly, including astrophysical explanations [44,45] and DM studies . The conclusions in these DM papers are consistent with ours.…”