A COMPARISON OF BROAD IRON EMISSION LINES IN ARCHIVAL DATA OF NEUTRON STAR LOW-MASS X-RAY BINARIES
A COMPARISON OF BROAD IRON EMISSION LINES IN ARCHIVAL DATA OF NEUTRON STAR LOW-MASS X-RAY BINARIES
复制标题
中子星低质量X射线双星档案数据中广泛铁发射线的比较
DOI：
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
D. Barret
中科院分区：
文献类型：
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作者：
E. Cackett;Jonathan M. Miller;R. Reis;A. Fabian;D. Barret
相对论X射线盘线在多中子星星低质量X射线双星中被发现，在质量尺度上与黑洞非常相似。这些谱线具有巨大的诊断能力，并已被用来限制恒星半径和磁场，通常发现与独立计时技术一致的值。在这里，我们比较了基于CCD的数据从朱雀与铁K线档案数据与基于气体的光谱仪。总的来说，我们发现EXOSAT、BeppoSAX和RXTE的气基谱线轮廓与朱雀的CCD数据之间具有很好的一致性，这表明所看到的宽谱线是谱线所固有的，而不是由于仪器问题而宽。然而，我们确实发现，当用高斯线轮廓拟合时，高斯线的宽度可以取决于低光谱分辨率仪器中的连续模型，尽管当不同模型拟合得同样好时，线宽通常一致。我们还证明了三个BeppoSAX观测显示的证据不对称线，相对论盘线模型提供了一个显着更好的拟合比高斯。我们使用后验预测p值方法和光谱的自举来测试这一点，以表明这种偏离高斯分布的情况不太可能偶然观察到。
Relativistic X-ray disklines have been found in multiple neutron star low-mass X-ray binaries, in close analogy with black holes across the mass scale. These lines have tremendous diagnostic power and have been used to constrain stellar radii and magnetic fields, often finding values that are consistent with independent timing techniques. Here, we compare CCD-based data from Suzaku with Fe K line profiles from archival data taken with gas-based spectrometers. In general, we find good consistency between the gas-based line profiles from EXOSAT, BeppoSAX, and RXTE and the CCD data from Suzaku, demonstrating that the broad profiles seen are intrinsic to the line and not broad due to instrumental issues. However, we do find that when fitting with a Gaussian line profile, the width of the Gaussian can depend on the continuum model in instruments with low spectral resolution, though when the different models fit equally well the line widths generally agree. We also demonstrate that three BeppoSAX observations show evidence for asymmetric lines, with a relativistic diskline model providing a significantly better fit than a Gaussian. We test this by using the posterior predictive p-value method, and bootstrapping of the spectra to show that such deviations from a Gaussian are unlikely to be observed by chance.
DOI：
10.1088/0004-637x/720/1/205
发表时间：
2009-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
E. Cackett
通讯作者：
E. Cackett