Likely detection of GeV γ-ray emission from pulsar wind nebula G32.64+0.53 with Fermi-LAT
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| Format: | Preprint |
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2024
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| _version_ | 1866929457898455040 |
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| author | Xiao, Yifan Wu, Keyao Fang, Jun |
| author_facet | Xiao, Yifan Wu, Keyao Fang, Jun |
| contents | In this study, we report the likely GeV γ-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 γ-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 γ-ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the γ-rays in TeV bands are likely generated by electrons/positrons within the nebula through Inverse Compton Scattering. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_06939 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Likely detection of GeV γ-ray emission from pulsar wind nebula G32.64+0.53 with Fermi-LAT Xiao, Yifan Wu, Keyao Fang, Jun High Energy Astrophysical Phenomena In this study, we report the likely GeV γ-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 γ-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 γ-ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the γ-rays in TeV bands are likely generated by electrons/positrons within the nebula through Inverse Compton Scattering. |
| title | Likely detection of GeV γ-ray emission from pulsar wind nebula G32.64+0.53 with Fermi-LAT |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.06939 |