The Vela pulsar and its pulsar wind nebula Vela-X using 13 years of Fermi-LAT Observations
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arXiv
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| Format: | Preprint |
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2025
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| author | Lange, Alexander Eagle, J. Kargaltsev, O. Kuiper, Lucien Hare, Jeremy |
| author_facet | Lange, Alexander Eagle, J. Kargaltsev, O. Kuiper, Lucien Hare, Jeremy |
| contents | We present results of more than 13 years of Fermi-LAT data analysis for the Vela pulsar from 60 MeV to 100 GeV and its pulsar wind nebula (PWN), Vela-X, for E > 1 GeV in the off-pulse phases. We find the Vela-X PWN can be best characterized using two extended components: a large radial Gaussian accompanied by an off-set, compact radial disk, both with a similar spectral index, Γ\sim 2.3. The common spectral properties support a common PWN origin, but a supernova remnant component is plausible for the compact radial disk. With an updated Vela-X model, the phase resolved spectral properties of the Vela pulsar are explored through a phase-resolved analysis. The phase-resolved spectral properties of the pulsar are presented, such as the SED peak energy E$_p$, the width of the SED at its peak, d$_p$, and the asymptotic (low-energy) spectral index, $Γ_0$, are presented. The best-fit spectral models for each LAT pulse peak (Peak 1 and Peak 2) are extrapolated to UV energies and compared to archival, phase-resolved spectra at UV, X-ray, soft γ-ray and TeV energies. We also discuss the physical implications of our modeling and the data comparisons. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_16687 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Vela pulsar and its pulsar wind nebula Vela-X using 13 years of Fermi-LAT Observations Lange, Alexander Eagle, J. Kargaltsev, O. Kuiper, Lucien Hare, Jeremy High Energy Astrophysical Phenomena We present results of more than 13 years of Fermi-LAT data analysis for the Vela pulsar from 60 MeV to 100 GeV and its pulsar wind nebula (PWN), Vela-X, for E > 1 GeV in the off-pulse phases. We find the Vela-X PWN can be best characterized using two extended components: a large radial Gaussian accompanied by an off-set, compact radial disk, both with a similar spectral index, Γ\sim 2.3. The common spectral properties support a common PWN origin, but a supernova remnant component is plausible for the compact radial disk. With an updated Vela-X model, the phase resolved spectral properties of the Vela pulsar are explored through a phase-resolved analysis. The phase-resolved spectral properties of the pulsar are presented, such as the SED peak energy E$_p$, the width of the SED at its peak, d$_p$, and the asymptotic (low-energy) spectral index, $Γ_0$, are presented. The best-fit spectral models for each LAT pulse peak (Peak 1 and Peak 2) are extrapolated to UV energies and compared to archival, phase-resolved spectra at UV, X-ray, soft γ-ray and TeV energies. We also discuss the physical implications of our modeling and the data comparisons. |
| title | The Vela pulsar and its pulsar wind nebula Vela-X using 13 years of Fermi-LAT Observations |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2506.16687 |