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The HAWC Collaboration has recently reported the detection of bright andspatially extended multi-TeV gamma-ray emission from Geminga, Monogem, and ahandful of other nearby, middle-aged pulsars. The angular profile of theemission observed from these pulsars is surprising, in that it implies thatcosmic-ray diffusion is significantly inhibited within ~25 pc of these objects,compared to the expectations of standard Galactic diffusion models. This raisesthe important question of whether the diffusion coefficient in the localinterstellar medium is also low, or whether it is instead better fit by themean Galactic value. Here, we utilize recent observations of the cosmic-rayelectron spectrum (extending up to ~20 TeV) by the H.E.S.S. Collaboration toshow that the local diffusion coefficient cannot be as low as it is in theregions surrounding Geminga and Monogem. Instead, we conclude that cosmic raysefficiently diffuse through the bulk of the local interstellar medium. Amongother implications, this further supports the conclusion that pulsarssignificantly contribute to the observed positron excess.

Measuring the Local Diffusion Coefficient with H.E.S.S. Observations of Very High-Energy Electrons