类星体超大质量黑洞组装产生的引力波信号
Gravitational Wave Signal from Assembling the Lightest Supermassive Black Holes
摘要：
我们计算的引力波信号从1000万太阳质量的超大质量黑洞（SMBH）的生长从第三族恒星的残余。这些低质量黑洞的组装特别重要，因为在这个质量范围内观测SMBH是激光干涉仪空间天线（LISA）的主要科学目标之一，这是NASA/ESA计划探测引力波的任务。我们使用高分辨率的宇宙学N体模拟来跟踪合并的主机暗物质晕的历史，并结合动力学摩擦，气体吸积和反馈的半解析方法模型的SMBHs的增长。我们发现，最常见的来源，在LISA带从我们的体积包括合并之间的中等质量的黑洞和SMBHs在红移小于2。这种类型的高质量比合并在引力波界还没有得到广泛的考虑;这种信号的检测和表征可能需要一种不同于SMBH合并或极端质量比吸入的技术。我们发现，这个新的LISA源的事件率依赖于气体吸积到黑洞的处方，以及在星系尺度上的动力学的精确模型;我们最好的估计是，在SMBH组装期间，在类似于本地群的体积内出现大约40个信噪比大于30的源--根据宇宙的体积推算，10年内大约观测到500个事件，尽管这一速率的准确性受到宇宙变化的影响。
英文摘要：
We calculate the gravitational wave signal from the growth of 10 million solar mass supermassive black holes (SMBH) from the remnants of Population III stars. The assembly of these lower mass black holes is particularly important because observing SMBHs in this mass range is one of the primary science goals for the Laser Interferometer Space Antenna (LISA), a planned NASA/ESA mission to detect gravitational waves. We use high resolution cosmological N-body simulations to track the merger history of the host dark matter halos, and model the growth of the SMBHs with a semi-analytic approach that combines dynamical friction, gas accretion, and feedback. We find that the most common source in the LISA band from our volume consists of mergers between intermediate mass black holes and SMBHs at redshifts less than 2. This type of high mass ratio merger has not been widely considered in the gravitational wave community; detection and characterization of this signal will likely require a different technique than is used for SMBH mergers or extreme mass ratio inspirals. We find that the event rate of this new LISA source depends on prescriptions for gas accretion onto the black hole as well as an accurate model of the dynamics on a galaxy scale; our best estimate yields about 40 sources with a signal-to-noise ratio greater than 30 occur within a volume like the Local Group during SMBH assembly -- extrapolated over the volume of the universe yields roughly 500 observed events over 10 years, although the accuracy of this rate is affected by cosmic variance.
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