Likely detection of GeV {\gamma}-ray emission from pulsar wind nebula G32.64+0.53 with Fermi-LAT

TL;DR

This study reports the detection of GeV gamma-ray emission from the pulsar wind nebula G32.64+0.53 using 14.7 years of Fermi-LAT data, modeling its broadband spectrum with a time-dependent one-zone model to explain the emission mechanisms.

Contribution

First detection of GeV gamma-ray emission from PWN G32.64+0.53, supported by spectral modeling linking multi-band observations to electron/positron processes.

Findings

Gamma-ray emission matches X-ray and TeV data.

Spectral energy distribution explained by synchrotron and inverse Compton processes.

Supports PWN origin of the gamma-ray source.

Abstract

In this study, we report the likely GeV {\gamma}-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 {\gamma}-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 {\gamma}-ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the {\gamma}-rays in TeV bands are likely generated by electrons/positrons within the nebula through Inverse Compton Scattering.