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• W3100308125 abstract "We present new observational and modeling results obtained for the Galactic nonthermal radio source G328.4+0.2. Using X-ray data obtained by XMM-Newton, we confirm that its X-ray emission is heavily absorbed, has a spectrum best fitted by a power-law model of photon index Γ = 2 with no evidence for a thermal component, comes from a region significantly smaller than the radio emission, and that the X-ray and radio emissions are significantly offset from each other. We also present the results of a new high-resolution (7'') 1.4 GHz image of G328.4+0.2 obtained using ATCA and a deep search for radio pulsations using the Parkes radio telescope. By comparing this 1.4 GHz image with a similar resolution image at 4.8 GHz, we find that the radio emission has a flat spectrum (α ≈ 0; Sν ∝ να). Additionally, we are able to limit the pseudoluminosity of any pulsar to L1400 ≡ S1400400d2 ≲ 30 mJy kpc2 for the central radio pulsar, assuming a distance of 17 kpc. In light of these observational results, we test whether G328.4+0.2 is a pulsar wind nebula or an SNR that contains a large pulsar wind nebula using a simple hydrodynamic model for the evolution of a pulsar wind nebula inside an SNR. As a result of this analysis, we conclude that G328.4+0.2 is a young (≲10,000 years old) pulsar wind nebula formed by a low magnetic field (≲1012 G) neutron star born spinning rapidly (≲10 ms) expanding into an undetected SNR formed by an energetic (≳1051 ergs), low ejecta mass (Mej ≲ 5 M☉) supernova explosion that occurred in a low-density (n ~ 0.03 cm-3) environment." @default.
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• W3100308125 date "2007-07-01" @default.
• W3100308125 modified "2023-09-24" @default.
• W3100308125 title "The Radio Emission, X‐Ray Emission, and Hydrodynamics of G328.4+0.2: A Comprehensive Analysis of a Luminous Pulsar Wind Nebula, Its Neutron Star, and the Progenitor Supernova Explosion" @default.
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• W3100308125 doi "https://doi.org/10.1086/518498" @default.
• W3100308125 hasPublicationYear "2007" @default.
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