The Vela pulsar and its pulsar wind nebula Vela-X using 13 years of Fermi-LAT Observations

Abstract

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, ${\Gamma }_0$, 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.

Accepted for publication in the Astrophysical Journal. 24 pages, 15 figures

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Cited by in corpus (2)

• GeV emission in the region of Vela: a new view of the supernova remnant
• Gamma-Ray Millisecond Pulsars: Off-pulse Emission Characteristics, Phase-Resolved Pseudo-Luminosity--Cutoff Energy Correlation, and High-energy Pulsed Emission