REVEALING THE STRUCTURE OF AN ACCRETION DISK THROUGH ENERGY-DEPENDENT X-RAY MICROLENSING
REVEALING THE STRUCTURE OF AN ACCRETION DISK THROUGH ENERGY-DEPENDENT X-RAY MICROLENSING
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通过能量相关的 X 射线微透镜揭示吸积盘的结构
DOI：
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发表时间：
2012
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影响因子：
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通讯作者：
J. Blackburne
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作者：
G. Chartas;C. S. Kochanek;X. Dai;D. Moore;A. Mosquera;J. Blackburne
我们展示了钱德拉 X 射线天文台对引力透镜类星体 RX J1131−1231 进行的监测观测结果。 X 射线观测计划采用相对较长的曝光时间，以便在 RX J1131−1231 图像的软（0.2-2 keV）和硬（2-10 keV）光曲线中寻找能量相关的微透镜。我们在图像 A 和 D 的 X 射线光曲线中检测到显着的微透镜，以及图像 D 的能量相关微透镜。当图像 D 放大时，软带的放大倍数似乎比硬带的放大倍数大 ∼1.3。这可以通过紧凑的、较软的光谱电晕与盘外产生更扩展、更硬的光谱反射分量之间的差异来解释。图像 D 中荧光铁线在光变曲线的三个连续时间平均阶段的演变支持了这一点。在第一个周期中，检测到 E = 6.35+0.14 − 0.14 keV 处的 Fe 线（置信度 >99%）。在第二个周期中，检测到两条 Fe 线，一条在 E = 5.50+0.03 − 0.08 keV 处（在 >99% 置信度下检测到），另一条在 E = 6.04+0.10 − 0.07 keV 处（在 >90% 置信度下勉强检测到），在第三个周期中，在 6.42+0.16 − 0.14 keV 处检测到一条加宽的 Fe 线（在>99% 置信度）。微透镜事件期间 Fe 谱线轮廓的这种演变与焦散线经过内盘时预期的线畸变一致，其中荧光 Fe 谱线的形状因广义相对论和多普勒效应而扭曲。
We present results from monitoring observations of the gravitationally lensed quasar RX J1131−1231 performed with the Chandra X-Ray Observatory. The X-ray observations were planned with relatively long exposures that allowed a search for energy-dependent microlensing in the soft (0.2–2 keV) and hard (2–10 keV) light curves of the images of RX J1131−1231. We detect significant microlensing in the X-ray light curves of images A and D, and energy-dependent microlensing of image D. The magnification of the soft band appears to be larger than that in the hard band by a factor of ∼1.3 when image D becomes more magnified. This can be explained by the difference between a compact, softer-spectrum corona that is producing a more extended, harder spectrum reflection component off the disk. This is supported by the evolution of the fluorescent iron line in image D over three consecutive time-averaged phases of the light curve. In the first period, an Fe line at E = 6.35+0.14 − 0.14 keV is detected (at >99% confidence). In the second period, two Fe lines are detected, one at E = 5.50+0.03 − 0.08 keV (detected at >99% confidence) and another at E = 6.04+0.10 − 0.07 keV (marginally detected at >90% confidence), and in the third period, a broadened Fe line at 6.42+0.16 − 0.14 keV is detected (at >99% confidence). This evolution of the Fe line profile during the microlensing event is consistent with the line distortion expected when a caustic passes over the inner disk where the shape of the fluorescent Fe line is distorted by general relativistic and Doppler effects.