Gravitational Lensing Size Scales for Quasars
Gravitational Lensing Size Scales for Quasars
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DOI：
10.1002/asna.201612313
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发表时间：
2015-09
影响因子：
0.9
通讯作者：
G. Chartas;C. Rhea;C. Kochanek;X. Dai;C. Morgan;J. Blackburne;B. Chen;A. Mosquera;C. D. O. Physics;Astronomy;College of Charleston;D. O. Astronomy;T. O. S. University;H. L. D. D. O. Physics-H.-L.-D.-D.-O.-Physics-2085307947;The University of Oklahoma;P. Department;U. S. N. Academy;Institute for Astronomy;U. Edinburgh
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文献类型：
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作者：
G. Chartas;C. Rhea;C. Kochanek;X. Dai;C. Morgan;J. Blackburne;B. Chen;A. Mosquera;C. D. O. Physics;Astronomy;College of Charleston;D. O. Astronomy;T. O. S. University;H. L. D. D. O. Physics-H.-L.-D.-D.-O.-Physics-2085307947;The University of Oklahoma;P. Department;U. S. N. Academy;Institute for Astronomy;U. Edinburgh
我们审查的结果，从我们的监测观测几个透镜类星体进行的光学，紫外线和X射线波段。多波长光变曲线的建模提供了对光学、UV和X射线发射区域的范围的约束。我们的分析的重要结果之一是，从微透镜分析推断的光学尺寸是显着大于理论薄盘估计预测。在少数情况下，我们还限制了大小-波长关系的斜率。我们的软，硬X射线发射区的类星体的大小限制表明，在我们的样本的一些对象的硬X射线发射区比软，在其他软发射区更紧凑。这种差异可能是我们样本中类星体中圆盘反射（更硬和更长）与日冕直接（更软和更紧凑）分量的相对强度的结果。最后，我们提出了几个强大的微透镜事件的分析，我们检测到的相对论Fe线轮廓的演变作为放大焦散横穿吸积盘。这些焦散交叉被用来提供约束的最内稳定圆轨道（ISCO）半径和吸积盘的类星体RX J1131-1231中的黑洞的倾角。（© 2016 WILEY-VCH Verlag GmbH & Co. KGaA，魏因海姆）
We review results from our monitoring observations of several lensed quasars performed in the optical, UV, and X-ray bands. Modeling of the multi-wavelength light curves provides constraints on the extent of the optical, UV, and X-ray emission regions. One of the important results of our analysis is that the optical sizes as inferred from the microlensing analysis are significantly larger than those predicted by the theoretical-thin-disk estimate. In a few cases we also constrain the slope of the size-wavelength relation. Our size constraints of the soft and hard X-ray emission regions of quasars indicate that in some objects of our sample the hard X-ray emission region is more compact than the soft and in others the soft emission region is smaller. This difference may be the result of the relative strengths of the disk-reflected (harder and extended) versus corona-direct (softer and compact) components in the quasars of our sample. Finally, we present the analysis of several strong microlensing events where we detect an evolution of the relativistic Fe line profile as the magnification caustic traverses the accretion disk. These caustic crossings are used to provide constraints on the innermost stable circular orbit (ISCO) radius and the accretion disk inclination angle of the black hole in quasar RX J1131–1231. (© 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)