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We investigate the observed spectrum of cosmic-ray electrons and positronsfrom astrophysical sources, especially pulsars, and the physical processes formaking the spectrum spiky or smooth via continuous and multipleelectron/positron injections. We find that (1) the average electron spectrumpredicted from nearby pulsars are consistent with PAMELA, Fermi and H.E.S.S.data. However, the ATIC/PPB-BETS peak around 500GeV is hard to produce by thesum of multiple pulsar contributions and requires a single (or a few) energeticpulsar(s). (2) A continuous injection produces a broad peak and a high energytail above the peak, which can constrain the source duration ($\lesssim 10^5$yrwith the current data). (3) The H.E.S.S. data in the TeV range suggest thatyoung sources with age less than $\sim 6 \times 10^4$yr are less energetic than$\sim 10^{48}{\rm erg}$. (4) We also expect a large dispersion in the TeVspectrum due to the small number of sources, that may cause the high energycutoff inferred by H.E.S.S. and potentially provide a smoking-gun for theastrophysical origin. These spectral diagnostics can be refined in the nearfuture by the CALET experiments to discriminate different astrophysical anddark matter origins.

Cosmic-Ray Electron Excess from Pulsars is Spiky or Smooth?: Continuous and Multiple Electron/Positron injections