X-Ray Monitoring of Gravitationally Lensed Radio-loud Quasars with Chandra
X-Ray Monitoring of Gravitationally Lensed Radio-loud Quasars with Chandra
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DOI：
10.3847/1538-4357/ab879b
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发表时间：
2019-09
期刊：
影响因子：
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通讯作者：
M. B. Doğruel;X. Dai;E. Guerras;M. Cornachione;C. Morgan
中科院分区：
文献类型：
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作者：
M. B. Doğruel;X. Dai;E. Guerras;M. Cornachione;C. Morgan
在这项工作中，我们计算了三个引力透镜射电响亮类星体，B 1422+231，MG J 0414 +0534和Q 0957+561的未分辨X射线发射区的大小，使用的X射线数据从钱德拉X射线天文台的成像和光谱分析相结合。我们在MG J 0414 +0534和Q 0957+561中初步检测到FeKα发射线，显著性超过95%，而在B 1422+231中未显著检测到FeKα发射。我们从吸收校正的计数率构建微分微透镜光曲线。我们随后对X射线微透镜光变曲线进行了微透镜分析，以基于贝叶斯或最大似然概率测量静止帧软（0.83-3.6 keV），硬（3.6-21.8 keV）和全（0.83-21.8 keV）带中的X射线源大小。对于B 1422+231，两种方法的大小彼此一致，（贝叶斯），11.81 ± 3.75（最大似然），其中。然而，对于MG J 0414 +0534和Q 0957+561，这两种方法产生了实质上不同的结果，这表明需要更频繁地采样具有更好的信噪比的数据来测量这两个对象的源大小。将获得的尺寸值与文献中的射电宁静样本进行比较，我们发现我们的结果与X射线源尺寸与中心超大质量黑洞质量的比例近似为RX <$MBH是一致的。我们的贝叶斯分析结果还表明，与无线电安静的类星体相比，无线电响亮的类星体往往具有更大的未分辨X射线发射尺寸，这表明更突出的喷流贡献。
In this work, we calculated the sizes of unresolved X-ray emission regions in three gravitationally lensed radio-loud quasars, B 1422+231, MG J0414+0534, and Q 0957+561, using a combination of imaging and spectral analysis on the X-ray data taken from the Chandra X-Ray Observatory. We tentatively detected FeKα emission lines in MG J0414+0534 and Q 0957+561 with over 95% significance, whereas, we did not significantly detect FeKα emission in B 1422+231. We constructed differential microlensing light curves from absorption corrected count rates. We subsequently performed a microlensing analysis on the X-ray microlensing light curves to measure the X-ray source sizes in rest frame soft (0.83–3.6 keV), hard (3.6–21.8 keV), and full (0.83–21.8 keV) bands, based on either Bayesian or maximum likelihood probabilities. For B 1422+231, sizes from the two methods are consistent with each other, (Bayesian), 11.81 ± 3.75 (maximum likelihood), where . However, for MG J0414+0534 and Q 0957+561, the two methods yield substantially different results suggesting that more frequently sampled data with better signal-to-noise ratio are needed to measure the source size for these two objects. Comparing the acquired size values with the radio-quiet sample in the literature we found that our results are consistent with X-ray source size scaling approximately as RX ∝ MBH with the mass of the central supermassive black hole. Our Bayesian analysis results also indicate that radio-loud quasars tend to have larger unresolved X-ray emission sizes compared to the radio-quiet ones, suggesting a more prominent jet contribution.