论文标题
揭示parsec尺度大规模黑洞二进制的宿主：形态和电磁签名
Unveiling the hosts of parsec-scale massive black hole binaries: morphology and electromagnetic signatures
论文作者
论文摘要
预计在结构形成的层次模型中，预计将形成parsec尺度的大型黑洞二进制二进制文件（MBHB）。即使已经设计了不同的观察策略来检测这些系统，但理论研究还是搜索和识别的进一步指南。在这项工作中，我们研究了主机属性和巨大黑洞重力的电磁特征，在Parsec-scales上，主要质量$ \ rm {>} \，10^7 \，m _ {\ odot} $。为此，我们通过使用半分析模型L-galaxies来构建一个全天空的灯酮，其中包括在其中进行了物理动机的处方，以形成MBHB的形成和演变。我们的预测表明，绝大多数MBHB都放置在具有经典凸起结构的螺旋星系中或椭圆星系中。此外，缩放关系随后是MBHB与单个巨大的黑洞没有区别。我们发现，Parsec-Scale MbHbs的职业最高可达到$ {\ sim} \，50 \％$在星系中，带有$ \ rm m_ {stellar} \，{>} \，{>} \，10^{11}}}} m_ {stellar} \，{<} \，10^{11} \，m _ {\ odot} $。我们的模型预计，大多数Parsec-Scale MBHB都是不平等的质量系统，并且位于$ z \，{\ sim} \，0.5 $，带有$ {\ sim} \，20 $ objects per $ \ rm verm verm v^2 $。但是，这些系统中的大多数都是不活动的，并且每$ \ rm deg^2 $只有$ 1 \，{ - } \，0.1 $对象具有一个电磁对应物，其砂光亮度超过$ 10^{43} $ erg/s。 Parsec-Scale MBHB的非常发光的阶段更为常见，在$ z \，{>} \，1 $中，但每$ \ rm deg^2 $ as $ {\ sillssim} \，0.01 $，0.01 $ at $ \ rm v^2 $ at $ \ rm l _ {\ rm l _ {\ rm bol} erg/s $。
Parsec-scale massive black hole binaries (MBHBs) are expected to form in hierarchical models of structure formation. Even though different observational strategies have been designed to detect these systems, a theoretical study is a further guide for their search and identification. In this work, we investigate the hosts properties and the electromagnetic signatures of massive black holes gravitationally bound on parsec-scales with primary mass $\rm {>}\,10^7\,M_{\odot}$. For that, we construct a full-sky lightcone by the use of the semi-analytical model L-Galaxies in which physically motivated prescriptions for the formation and evolution of MBHBs have been included. Our predictions show that the large majority of the MBHBs are placed either in spiral galaxies with a classical bulge structure or in elliptical galaxies. Besides, the scaling relations followed by MBHBs are indistinguishable from the ones of single massive black holes. We find that the occupation fraction of parsec-scale MBHBs reaches up to ${\sim}\,50\%$ in galaxies with $\rm M_{stellar}\,{>}\,10^{11}\, M_{\odot}$ and drops below 10\% for $\rm M_{stellar}\,{<}\,10^{11}\, M_{\odot}$. Our model anticipates that the majority of parsec-scale MBHBs are unequal mass systems and lie at $z\,{\sim}\,0.5$, with ${\sim}\,20$ objects per $\rm deg^2$ in the sky. However, most of these systems are inactive, and only $1\,{-}\,0.1$ objects per $\rm deg^2$ have an electromagnetic counterpart with a bolometric luminosity in excess of $10^{43}$ erg/s. Very luminous phases of parsec-scale MBHBs are more common at $z\,{>}\,1$ but the number of binaries per $\rm deg^2$ is ${\lesssim}\,0.01$ at $\rm L_{\rm bol}\,{>}\,10^{45} \rm erg/s$.
