NuSTAR and XMM-Newton Observations of PSR J1930+1852 and Its Pulsar Wind Nebula

Abstract

Synchrotron X-ray emission from a pulsar wind nebula (PWN) is a sensitive probe of its magnetic field and high-energy particle population. Here we analyze contemporaneous NuSTAR and XMM-Newton observations of the PWN G54.1+0.3, powered by pulsar PSR J1930+1852. We also present a preliminary timing analysis of the central pulsar PSR J1930+1852 and analyze its X-ray pulse profiles in different energy bands. We detect X-ray emission from the combined pulsar and PWN system up to $\approx 70$ keV, while emission from the PWN itself has been detected up to $\approx 30$ keV, with a photon index $\Gamma$ increasing from $\sim 1.9$ to $\sim 2.4$ with photon energy between 3 and 30 keV. PWN G54.1+0.3's X-ray spectrum is consistent with a broken power law, with break energy $E_{\mathrm{break}}\approx 5$ keV, consistent with synchrotron cooling of a single power-law particle spectrum. The best-fit broadband spectral energy distribution model after the inclusion of this new spectral data indicates a maximum particle $E_{\max }\sim 400$ TeV. We discuss PSR J1930+1852 and PWN G54.1+0.3 in the context of other PWNe powered by young energetic pulsars.

arXiv comment12 pages, 5 figures, accepted for publication in ApJ

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Cited by in corpus (1)

• New Hard X-Ray and Multiwavelength Study of the PeVatron Candidate PWN G0.9+0.1 in the Galactic Center Region