论文标题
超级巨头快速X射线瞬态IGR J16479-4514与XMM-Newton和Integrant Antegrale一起研究的超级X射线瞬态IGR J16479-4514的粉尘冰球光环和巨大的硬X射线耀斑
Dust-scattering halo and giant hard X-ray flare from the Supergiant Fast X-ray Transient IGR J16479-4514 investigated with XMM-Newton and INTEGRAL
论文作者
论文摘要
我们报告了XMM-Newton分析的结果以及IGR J16479-4514的积分数据。未发表的XMM-Newton观察于2012年进行，发生在源食源期间。未从源中检测到类似点的X射线发射，相反，延伸的X射线发射清楚地检测到尺寸距离兼容，与源X射线发射产生的灰尘散射光环，然后由其同伴供体恒星黯然失色。 The diffuse emission of the dust-scattering halo could be observed without any contamination from the central point X-ray source, compared to a previous XMM-Newton observation published in 2008. Our comprehensive analysis of the 2012 unpublished spectrum of the diffuse emission as well as of the 2008 re-analysed spectra extracted from three adjacent time intervals and different extraction regions (optimized for point-like and extended emission) allowed us to clearly在2008年食物期间，将散射光谱频谱与残留点样发射的散射光谱。此外，在2008年检测到的点样发射可以分别分为两个分别归因于从源的直接发射到恒星风中的散射。从档案未出版的积分数据中，我们确定了非常强的（3 $ \ times $ 10 $^{ - 8} $ erg cm $^{ - 2} $ s $ s $^{ - 1} $）和快速（25分钟的耀斑），该耀斑被分类为巨大的X射线闪光s $^{ - 1} $。来自SFXT的巨型X射线耀斑非常罕见，迄今为止，仅报告了另一种来源。我们提出了一个物理场景，以解释IGR J16479-4514的起源。
We report results from the analysis of XMM-Newton and INTEGRAL data of IGR J16479-4514. The unpublished XMM-Newton observation, performed in 2012, occurred during the source eclipse. No point-like X-ray emission was detected from the source, conversely extended X-ray emission was clearly detected up to a size distance compatible with a dust scattering halo produced by the source X-ray emission before being eclipsed by its companion donor star. The diffuse emission of the dust-scattering halo could be observed without any contamination from the central point X-ray source, compared to a previous XMM-Newton observation published in 2008. Our comprehensive analysis of the 2012 unpublished spectrum of the diffuse emission as well as of the 2008 re-analysed spectra extracted from three adjacent time intervals and different extraction regions (optimized for point-like and extended emission) allowed us to clearly disentangle the scattering halo spectrum from the residual point-like emission during the 2008 eclipse. Moreover, the point-like emission detected in 2008 could be separated into two components attributed to the direct emission from the source and to scattering in the stellar wind, respectively. From archival unpublished INTEGRAL data, we identified a very strong (3$\times$10$^{-8}$ erg cm$^{-2}$ s$^{-1}$) and fast (25 minutes duration) flare which was classified as giant hard X-ray flare since the measured peak-luminosity is 7$\times$10$^{37}$ erg s$^{-1}$. Giant X-ray flares from SFXTs are very rare, to date only one has been reported from a different source. We propose a physical scenario to explain the origin in the case of IGR J16479-4514.
