Broadband X-ray Spectroscopy & Multi-Wavelength Modeling of the Pulsar Wind Nebula in HESS J1640-465

Pulsar Wind Nebulae (PWNe) are often studied to infer the properties of their progenitor supernova, associated neutron star, and their pulsar wind as they are hard to measure directly. Currently, this is best achieved by using an evolutionary model of a spherical PWN inside a SNR to fit the observed dynamical and radiative properties of these PWNe. Connected to that, PWNe are considered among the Galactic PeVatron candidates; objects that can accelerate particles up to PeV energies. HESS J1640-465, by virtue among the most luminous TeV sources in the galaxy, must accelerate a considerable number of leptons to PeV energies, and its high spin-down luminosity of 4.4 * 10³⁶ ergs/s suggest these particles are produced in its PWN. In this talk, I will present new measurements of the X-ray properties of this PWN between 3-30 keV, finding, for the first time, evidence for spectral softening and decreasing unabsorbed flux as we go to higher photon energies. By fitting the broadband properties of our system, we find a short spin-down time scale, a wind magnetization of a higher than average value, a strong PWN magnetic field and maximum electron energy up to ~ 1.5 PeV, suggesting HESS J1640-465 is a PeVatron candidate.