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One of the most essential but uncertain processes for producing cosmic-rays(CRs) and their spectra is how accelerated particles escape into theinterstellar space. We propose that the CR electron spectra at >~TeV energy canprovide a direct probe of the CR escape complementary to the CR nuclei andgamma-rays. We calculate the electron spectra from a young pulsar embedded inthe supernova remnant (SNR), like Vela, taking into account theenergy-dependent CR escape. SNRs would accelerate and hence confine particleswith energy up to 10^{15.5}eV. Only energetic particles can escape first, whilethe lower energy particles are confined and released later. Then the observedelectron spectrum should have a low energy cutoff whose position marks the ageof the pulsar/SNR. The low energy cutoff is observable in the $\gtrsim {\rmTeV}$ energy window, where other contaminating sources are expected to be fewdue to the fast cooling of electrons. The spectrum looks similar to a darkmatter annihilation line if the low energy cutoff is close to the high energyintrinsic or cooling break. The future experiments such as CALET and CTA arecapable of directly detecting the CR escape features toward revealing theorigin of CRs.

TeV Electron Spectrum for Probing Cosmic-Ray Escape from a Supernova Remnant