Likely Detection of GeV γ-Ray Emission from Pulsar Wind Nebula G32.64+0.53 with Fermi-LAT

被引：1

作者：

Xiao, Yifan ^{[1
]}

Wu, Keyao ^{[1
]}

Fang, Jun ^{[1
]}

机构：

[1] Yunnan Univ, Sch Phys & Astron, Dept Astron, Key Lab Astroparticle Phys Yunnan Prov, Kunming 650091, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2024年 / 972卷 / 01期

关键词：

LARGE-AREA TELESCOPE; HESS; TEV; POPULATION; EVOLUTION; CATALOG; DISCOVERY; FIELD; HAWC;

D O I：

10.3847/1538-4357/ad6563

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 yr of data from the Fermi Large Area Telescope 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 multiband nonthermal 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 ICS.

引用

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