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ROSAT and ASCA observations of the Crab-Like Supernova Remnant N157B in the Large Magellanic Cloud | Q. Daniel Wang
; Eric V. Gotthelf
; | Date: |
9 Aug 1997 | Subject: | astro-ph | Abstract: | We report the results of ROSAT and ASCA X-ray observations of the supernova remnant N157B (or 30 Dor B, SNR 0539-69.1) in the Large Magellanic Cloud. For comparison, we also briefly describe the results on SNR 0540-69.3, the only confirmed Crab-like remnant in the Cloud. The X-ray emission from N157B can be decomposed into a bright comet-shaped feature, superimposed on a diffuse emission region of a dimension $sim 20$ pc. The flat and nearly featureless spectrum of the remnant is distinctly different from those of young shell-like remnants, suggesting a predominantly Crab-like nature of N157B. Characterized by a power law with an energy slope $sim 1.5$, the spectrum of N157B above $sim 2$ keV is, however, considerably steeper than that of SNR 0540-69.3, which has a slope of $sim 1.0$. At lower energies, the spectrum of N157B presents marginal evidence for emission lines, which if real most likely arise in hot gas of the diffuse emission region. The hot gas has a characteristic thermal temperature of 0.4-0.7 keV. No significant periodic signal is detected from N157B in the period range of $3 imes 10^{-3}-2000$ s. The pulsed fraction is $lesssim 9%$ (99% confidence) in the $2-7$ keV range. We discuss the nature of the individual X-ray components. In particular, we suggest that the synchrotron radiation of relativistic particles from a fast-moving ($sim 10^3 km s^{-1}$) pulsar explains the size, morphology, spectrum, and energetics of the comet-shaped X-ray feature. We infer the age of the remnant as $sim 5 imes 10^3$ yrs. The lack of radio polarization of the remnant may be due to Faraday dispersion by foreground ion{H}{2} gas. | Source: | arXiv, astro-ph/9708087 | Services: | Forum | Review | PDF | Favorites |
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