NuSTAR observations of Mrk 766: distinguishing reflection from absorption
NuSTAR observations of Mrk 766: distinguishing reflection from absorption
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DOI：
10.1093/mnras/sty2081
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发表时间：
2018-07
影响因子：
4.8
通讯作者：
D. Buisson;M. Parker;E. Kara;R. Vasudevan;A. Lohfink;C. Pinto;A. Fabian;D. Ballantyne;S. Boggs;F. Christensen;W. Craig;D. Farrah;C. Hailey;F. Harrison;C. Ricci;D. Stern;D. Walton;W. Zhang
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作者：
D. Buisson;M. Parker;E. Kara;R. Vasudevan;A. Lohfink;C. Pinto;A. Fabian;D. Ballantyne;S. Boggs;F. Christensen;W. Craig;D. Farrah;C. Hailey;F. Harrison;C. Ricci;D. Stern;D. Walton;W. Zhang
我们提出了两个新的努斯塔观测的窄线塞弗特1（NLS 1）星系Mrk 766和以前提出的两个方案，以解释其光谱和其他NLS 1的限制：相对论反射和部分覆盖。努斯塔光谱显示出强的硬（>15 keV）X射线过剩，而同时由XMM-牛顿提供的观测之一的软X射线覆盖限制了源中的电离吸收。纯反射模型需要一个在中等倾角（i=46^（+1）_（-4）<$）下观察的高自旋（a > 0.92）黑洞。纯粹的部分覆盖模型需要极端的参数：在一次观测中，主连续谱的截止值非常低（22^（+7）_（-5）keV），并且内在X射线发射必须提供大部分（75%）的热光度。允许部分覆盖和反射的混合模型提供了更合理的吸收参数，并放松了对反射参数的约束。在铁K带周围和包括康普顿峰在内的高能量处，分数变化率降低，这表明反射发射的变化比连续谱小。
We present two new NuSTAR observations of the narrow-line Seyfert 1 (NLS1) galaxy Mrk 766 and give constraints on the two scenarios previously proposed to explain its spectrum and that of other NLS1s: relativistic reflection and partial covering. The NuSTAR spectra show a strong hard (>15 keV) X-ray excess, while simultaneous soft X-ray coverage of one of the observations provided by XMM–Newton constrains the ionized absorption in the source. The pure reflection model requires a black hole of high spin (a > 0.92) viewed at a moderate inclination (i=46^(+1)_(−4)∘). The pure partial covering model requires extreme parameters: the cut-off of the primary continuum is very low (22^(+7)_(−5) keV) in one observation and the intrinsic X-ray emission must provide a large fraction (75 per cent) of the bolometric luminosity. Allowing a hybrid model with both partial covering and reflection provides more reasonable absorption parameters and relaxes the constraints on reflection parameters. The fractional variability reduces around the iron K band and at high energies including the Compton hump, suggesting that the reflected emission is less variable than the continuum.