X-ray observations of supernova remnant G54.1+0.3: X-ray spectrum and the discovery of an X-ray jet

Abstract

We present in this paper analyses of the $ROSAT$ PSPC and $ASCA$ SIS and GIS observations of the Crab-like supernova remnant (SNR) G54.1+0.3. Its spectrum obtained by $ROSAT$ PSPC favors a power law model with a photon index of -0.8${}_{-2.0}^{+0.8}$, absorbed energy flux in 0.1-2.4 keV of 1.0$\times 10^{-12}$ erg cm${}^{-2}$ s${}^{-1}$, and absorption column density of 12.3${}_{-3.2}^{+8.0}\times 10^{21}$ cm${}^{-2}$. $ASCA$ SIS observation shows that its spectrum can also be best fitted with power law model. The fitted parameters are, photon index -1.9${}_{-0.2}^{+0.1}$, absorbed energy flux in 0.7-2.1 keV 6.5$\times 10^{-13}$ erg cm${}^{-2}$ s${}^{-1}$, and column density 17.9${}_{-2.5}^{+2.8}\times 10^{21}$ cm${}^{-2}$. The high absorption column density indicates a distance similar to the radius of the galaxy. The 0.1-2.4 keV X-ray luminosity of G54.1+0.3 is 3.2$\times 10^{33}$$d_{10}^2$ erg s${}^{-1}$, where $d_{10}$ is the distance in 10 kpc. With an image restoration method we have obtained high spatial resolution X-ray image of the remnant, which clearly shows an X-ray jet pointing to the northeast with a length about 40$\arcsec$ from the center of the nebula. Its X-ray luminosity in 0.1-2.4 keV is about 5.1$\times 10^{32}$$d_{10}^2$ erg s${}^{-1}$. The X-ray jet is consistent with the radio extension to the northeast in both direction and position. We propose that the X-ray jet is connected with the pulsar assumed to exist in the remnant.

6 pages, 6 figures included, submitted to A&A

References in corpus (3)

• The Distance to the Vela Supernova Remnant
• ROSAT and ASCA observations of the Crab-Like Supernova Remnant N157B in the Large Magellanic Cloud
• Reconstruction of Objects by Direct Demodulation

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• The soft gamma-ray pulsar population: an high-energy overview
• Discovery of a 136 millisecond radio and X-ray pulsar in SNR G54.1+0.3
• Study of Four Young TeV Pulsar Wind Nebulae with a Spectral Evolution Model
• A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3
• Deep Chandra Observations of the Crab-like Pulsar Wind Nebula G54.1+0.3 and Spitzer Spectroscopy of the Associated Infrared Shell
• XMM-Newton spectral analysis of the Pulsar Wind Nebula within the composite SNR G0.9+0.1
• The Chandra Detection of Galactic Center X-ray Features G359.89-0.08 and G359.54+0.18
• Arecibo HI Absorption Measurements of Pulsars and the Electron Density at Intermediate Longitudes in the First Galactic Quadrant
• The Properties of the Progenitor Supernova, Pulsar Wind, and Neutron Star inside PWN G54.1+0.3
• Dust formation in embryonic pulsar-aided supernova remnants
• SNR G54.1+0.3, a PeVatron candidate unveiled by LHAASO
• Particle acceleration to PeV energies in Pulsar Wind Nebula: a two zone model