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HAWC J1826-128 is one of the brightest Galactic TeV gamma-ray sourcesdetected by the High Altitude Water Cherenkov (HAWC) Observatory, with photonenergies extending up to nearly $\sim$100 TeV. This HAWC source spatiallycoincides with the H.E.S.S. TeV source HESS J1826-130 and the "Eel" pulsar windnebula (PWN), which is associated with the GeV pulsar PSR J1826-1256. In theX-ray band, Chandra and XMM-Newton revealed that the Eel PWN is composed ofboth a compact nebula ($\sim$15") and diffuse X-ray emission($\sim$6'$\times$2') extending away from the pulsar. Our NuSTAR observationdetected hard X-ray emission from the compact PWN up to $\sim$20 keV andevidence of the synchrotron burn-off effect. In addition to the spatialcoincidence between HESS J1826-130 and the diffuse X-ray PWN, ourmulti-wavelength spectral energy distribution (SED) analysis using X-ray andgamma-ray data establishes a leptonic origin of the TeV emission associatedwith the Eel PWN. Furthermore, our evolutionary PWN SED model suggests (1) alow PWN B-field of $\sim$1 $\mu$G, (2) a significantly younger pulsar age ($t\sim5.7$ kyr) than the characteristic age ($\tau= 14.4$ kyr) and (3) a maximumelectron energy of $E_{max} = 2$ PeV. The low B-field as well as the putativesupersonic motion of the pulsar may account for the asymmetric morphology ofthe diffuse X-ray emission. Our results suggest that the Eel PWN may be aleptonic PeVatron particle accelerator powered by the $\sim$6-kyr-old pulsarPSR J1826-1256 with a spin-down power of $3.6 \times 10^{36}$ erg s$^{-1}$.

The Eel Pulsar Wind Nebula: a PeVatron-Candidate Origin for HAWC J1826-128 and HESS J1826-130