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In this study, we report the likely GeV -ray emissions originating from the pulsar PSR J1849-0001's pulsar wind nebula (PWN) G32. 64+0. 53. Our analysis covers approximately 14. 7 years of data from the Fermi Large Area Telescope (Fermi-LAT) Pass 8. The position of the source and its spectrum matches those in X-ray and TeV energy bands, so we propose that the GeV -ray source is indicative of PWN G32. 64+0. 53. We interpret the broadband spectral energy distribution (SED) using a time-dependent one-zone model, which assumes that the multi-band non-thermal emission of the target source can be generated by synchrotron radiation and inverse Compton scattering (ICS) of the electrons/positrons. Our findings demonstrate that the model substantially elucidates the observed SED. These results lend support to the hypothesis that the -ray source originates from the PWN G32. 64+0. 53 powered by PSR J1849-0001. Furthermore, the -rays in TeV bands are likely generated by electrons/positrons within the nebula through Inverse Compton Scattering.
Xiao et al. (Tue,) studied this question.