NuSTAR Observations of Galactic Center Pulsar Wind Nebula G0.9+0.1

Pulsar Wind Nebulae (PWNe) are efficient particle accelerators, emitting synchrotron radiation in the radio and X-ray bands and are some of the most powerful TeV gamma-ray emitters in our Galaxy. However, the underlying acceleration processes are not fully known. G0.9+0.1 is a composite-type supernova remnant (SNR) and pulsar wind nebula (PWN) located in the direction of the Galactic Center and has been long studied in the <10 keV X-ray regime. G0.9+0.1 also has coincident gamma-ray emission detected by HESS, CTA, and VERITAS, making the PWN an ideal candidate for probing the physical mechanisms responsible for accelerating high-energy particles. We present here results from the newly-acquired NuSTAR observation of G0.9+0.1, including spatial and spectral analysis of the >10 keV emission. The hard NuSTAR X-ray emission also provides coverage in a crucial regime of the broad-band spectral energy distribution (SED). We present our best-fit SED results and the resultant model parameter constraints which shed light on the hadronic or leptonic emission from this PeVatron candidate.