2026ApJ...998..230B

We present a new X-ray study and multiwavelength spectral energy distribution (SED) modeling of the young pulsar wind nebula (PWN) powered by the energetic pulsar PSR J1747-2809, inside the composite supernova remnant (SNR) G0.9+0.1, located in the Galactic center region. The source is detected by NuSTAR up to 30 keV with evidence for the synchrotron burnoff effect in the changing spatial morphology with increasing energy. The broadband 2-30 keV spectrum of PWN G0.9+0.1 is modeled by a single power law with photon index Γ = 2.11 ± 0.07. We combined the new X-ray data with multiwavelength observations in radio, GeV, and TeV gamma rays and modeled the SED, applying one-zone and multizone leptonic models. The comparison of the models is successful, as we obtained physically compatible results in the two cases. Through the one-zone model, we constrain the age of the system to ∼2.2 kyr, as well as reproduce the observed PWN and SNR radio sizes. In both the one-zone and multizone leptonic models, the electron injection spectrum is well described by a single power law with spectral index p ∼ 2.6 and a maximum electron energy of ∼2 PeV, suggesting the source could be a leptonic PeVatron candidate. We estimate the average magnetic field to be B_PWN ∼ 20 μG. We also report the serendipitous NuSTAR detection of renewed X-ray activity from the very faint X-ray transient XMMU J174716.1-281048 and characterize its spectrum.