THE REFLECTION COMPONENT FROM CYGNUS X-1 IN THE SOFT STATE MEASURED BY NuSTAR AND SUZAKU
THE REFLECTION COMPONENT FROM CYGNUS X-1 IN THE SOFT STATE MEASURED BY NuSTAR AND SUZAKU
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DOI：
10.1088/0004-637x/780/1/78
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发表时间：
2013-10
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通讯作者：
J. Tomsick;M. Nowak;M. Parker;Jonathan M. Miller;A. Fabian;F. Harrison;M. Bachetti;D. Barret;S. Boggs;F. Christensen;W. Craig;K. Forster;F. Fuerst;B. Grefenstette;C. Hailey;A. King;K. Madsen;L. Natalucci;K. Pottschmidt;R. Ross;D. Stern;D. Walton;J. Wilms;Will Zhang
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作者：
J. Tomsick;M. Nowak;M. Parker;Jonathan M. Miller;A. Fabian;F. Harrison;M. Bachetti;D. Barret;S. Boggs;F. Christensen;W. Craig;K. Forster;F. Fuerst;B. Grefenstette;C. Hailey;A. King;K. Madsen;L. Natalucci;K. Pottschmidt;R. Ross;D. Stern;D. Walton;J. Wilms;Will Zhang
黑洞双星Cygnus X-1是在2012年底由核光谱望远镜阵列（NuSTAR）和Suzaku观测到的，提供了1-300 keV范围内的光谱覆盖。该源处于软态，具有多温黑体、幂律、反射分量以及系统中高电离物质的吸收。NuSTAR的高通量允许对复杂的铁线区域以及反射成分的其余部分进行非常高质量的测量。铁线明显变宽，并被相对论模糊模型很好地描述，这为约束黑洞旋转提供了机会。尽管自旋约束在某种程度上取决于所使用的连续介质模型，但对于所有能很好地描述光谱的模型，我们都得到了一个* > 0.83。然而，我们的光谱拟合都没有给出与最近报道的Cyg X-1双星值一致的盘倾角。这可能表明轨道平面与内部吸积盘（即翘曲吸积盘）之间存在>13°的错位，或者光谱模型中存在物理缺失。
The black hole binary Cygnus X-1 was observed in late 2012 with the Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku, providing spectral coverage over the ∼1–300 keV range. The source was in the soft state with a multi-temperature blackbody, power law, and reflection components along with absorption from highly ionized material in the system. The high throughput of NuSTAR allows for a very high quality measurement of the complex iron line region as well as the rest of the reflection component. The iron line is clearly broadened and is well described by a relativistic blurring model, providing an opportunity to constrain the black hole spin. Although the spin constraint depends somewhat on which continuum model is used, we obtain a* > 0.83 for all models that provide a good description of the spectrum. However, none of our spectral fits give a disk inclination that is consistent with the most recently reported binary values for Cyg X-1. This may indicate that there is a >13° misalignment between the orbital plane and the inner accretion disk (i.e., a warped accretion disk) or that there is missing physics in the spectral models.