Lorentz factor distribution of blazars from the optical Fundamental plane of black hole activity
Lorentz factor distribution of blazars from the optical Fundamental plane of black hole activity
复制标题
黑洞活动光学基本面的耀变体洛伦兹因子分布
DOI：
10.1093/mnras/stw1321
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发表时间：
2016
影响因子：
4.8
通讯作者：
H. Falcke
中科院分区：
文献类型：
--
作者：
P. Saikia;Elmar Kording;H. Falcke
Blazar辐射主要是由一个相对论性喷流，它可以在第一近似模型使用两个内在参数-洛伦兹因子$\Gamma$和视角$\theta$。由于相对论效应，Blazar喷流观测经常被波束化，使对这些内在性质的理解变得复杂。估算耀变体洛伦兹因子的最常用方法是估算视喷流速度和多普勒波束因子。我们提出了一种新的和独立的方法来构建耀变体洛伦兹因子分布，使用黑洞活动的光学基平面。光学基本平面是由超大质量黑洞和X射线双星在[OIII]线光度，射电光度和黑洞质量提供的3D空间中延伸的平面。我们使用从光学基本平面获得的内禀射电光度来约束VLBA成像和偏振测量巡天（VIPS）blazar样本的增强参数。我们发现一个耀变体的整体洛伦兹因子分布的形式的幂律为$N（\Gamma）\propto \Gamma^{-2.1 \pm 0.4}$的$\Gamma$范围为1至40。我们还讨论了耀变体的视角分布和我们的结果对输入参数的依赖性。
Blazar radiation is dominated by a relativistic jet which can be modeled at first approximation using just two intrinsic parameters - the Lorentz factor $\Gamma$ and the viewing angle $\theta$. Blazar jet observations are often beamed due to relativistic effects, complicating the understanding of these intrinsic properties. The most common way to estimate blazar Lorentz factors needs the estimation of apparent jet speeds and Doppler beaming factors. We present a new and independent method of constructing the blazar Lorentz factor distribution, using the optical fundamental plane of black hole activity. The optical fundamental plane is a plane stretched out by both the supermassive black holes and the X-ray binaries, in the 3D space provided by their [OIII] line luminosity, radio luminosity and black hole mass. We use the intrinsic radio luminosity obtained from the optical fundamental plane to constrain the boosting parameters of the VLBA Imaging and Polarimetry Survey (VIPS) blazar sample. We find a blazar bulk Lorentz factor distribution in the form of a power law as $N(\Gamma) \propto \Gamma^{-2.1 \pm 0.4}$ for the $\Gamma$ range of 1 to 40. We also discuss the viewing angle distribution of the blazars and the dependence of our results on the input parameters.