Pre-DECIGO can get the smoking gun to decide the astrophysical or cosmological origin of GW150914-like binary black holes
Pre-DECIGO can get the smoking gun to decide the astrophysical or cosmological origin of GW150914-like binary black holes
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DOI：
10.1093/ptep/ptw127
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发表时间：
2016-07
影响因子：
3.5
通讯作者：
Takashi Nakamura;M. Ando;T. Kinugawa;H. Nakano;K. Eda;S. Sato;M. Musha;T. Akutsu;Takahiro Tanaka;N. Seto;N. Kanda;Y. Itoh
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文献类型：
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作者：
Takashi Nakamura;M. Ando;T. Kinugawa;H. Nakano;K. Eda;S. Sato;M. Musha;T. Akutsu;Takahiro Tanaka;N. Seto;N. Kanda;Y. Itoh
Pre-DECIGO由三个以等边三角形排列的航天器组成，臂长100公里，在地球表面上空2000公里的轨道上运行。预计发射日期将在2020年代后期。Pre-DECIGO有一个明确的目标：像GW 150914和GW 151226这样的双黑洞（BBH）。Pre-DECIGO可以检测到$\sim 30M_\odot-30M_\odot$ BBH合并，最高红移为$z\sim 30$。累积事件率是$\sim 1.8\times 10^{5}\，{\rm events~yr^{-1}}$在像GW 150914这样的BBH的Pop III起源模型中，它在$z\sim 10$处饱和，而在原始BBH（PBBH）模型中，累积事件率是$ \sim 3\times 10^{4}\，{\rm事件~ yr^{-1}}$在$z=30$即使只有$0. 1\%$的暗物质组成的PBH，它仍然增加在$z=30$。在BBH的Pop I/II模型中，累积事件率为$（3-10）\times 10 ^{5}\，{\rm events~ yr^{-1}}$，在z \sim 6$时饱和。我们提出的轨道精度，无阻力技术，激光功率，频率稳定性和干涉仪测试质量的要求。对于像GW 150914这样的BBH，在1Gpc下，SNR$\sim 90$通过在$0.01- 100 $Hz频带中的Pre-DECIGO的定义来实现。Pre-DECIGO可以测量质谱和合并率的z依赖性，以区分各种型号的BBH，如GW 150914。Pre-DECIGO还可以在合并前一天左右预测z=0.1$的BBH方向，精度为$\sim 0.3\，{\rm deg}^2$，合并时间精度为$\sim 1$s，以便当时进一步发展的地基GW探测器以及电磁跟踪观测可以提前为合并的探测做好准备。对于中等质量的BBH在一个大的红移$z > 10$，合并后的QNM频率可以在Pre-DECIGO带内，使振铃尾巴也可以检测到证实爱因斯坦广义相对论与SNR$\sim 35$。[删节]
Pre-DECIGO consists of three spacecraft arranged in an equilateral triangle with 100km arm lengths orbiting 2000km above the surface of the earth. It is hoped that the launch date will be in the late 2020s. Pre-DECIGO has one clear target: binary black holes (BBHs) like GW150914 and GW151226. Pre-DECIGO can detect $\sim 30M_\odot-30M_\odot$ BBH mergers up to redshift $z\sim 30$. The cumulative event rate is $\sim 1.8\times 10^{5}\,{\rm events~yr^{-1}}$ in the Pop III origin model of BBHs like GW150914, and it saturates at $z\sim 10$, while in the primordial BBH (PBBH) model, the cumulative event rate is $ \sim 3\times 10^{4}\,{\rm events~ yr^{-1}}$ at $z=30$ even if only $0.1\%$ of the dark matter consists of PBHs, and it is still increasing at $z=30$. In the Pop I/II model of BBHs, the cumulative event rate is $(3-10)\times10^{5}\,{\rm events~ yr^{-1}}$ and it saturates at $z \sim 6$. We present the requirements on orbit accuracy, drag free techniques, laser power, frequency stability, and interferometer test mass. For BBHs like GW150914 at 1Gpc, SNR$\sim 90$ is achieved with the definition of Pre-DECIGO in the $0.01-100$Hz band. Pre-DECIGO can measure the mass spectrum and the $z$-dependence of the merger rate to distinguish various models of BBHs like GW150914. Pre-DECIGO can also predict the direction of BBHs at $z=0.1$ with an accuracy of $\sim 0.3\,{\rm deg}^2$ and a merging time accuracy of $\sim 1$s at about a day before the merger so that ground-based GW detectors further developed at that time as well as electromagnetic follow-up observations can prepare for the detection of merger in advance. For intermediate mass BBHs at a large redshift $z > 10$, the QNM frequency after the merger can be within the Pre-DECIGO band so that the ringing tail can also be detectable to confirm the Einstein theory of general relativity with SNR$\sim 35$. [abridged]