Systematic bias on the inspiral-merger-ringdown consistency test due to neglect of orbital eccentricity
Systematic bias on the inspiral-merger-ringdown consistency test due to neglect of orbital eccentricity
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DOI：
10.1103/physrevd.107.024009
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发表时间：
2022-07
影响因子：
5
通讯作者：
S. Bhat;P. Saini;Marc Favata;K. Arun
中科院分区：
文献类型：
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作者：
S. Bhat;P. Saini;Marc Favata;K. Arun
吸气-合并-振铃 (IMR) 一致性测试检查双黑洞合并残余物的最终质量和最终自旋的一致性，通过波形的吸气和合并-振铃部分独立推断。由于双星在进入地面探测器频段时预计会接近圆形，因此广义相对论（GR）测试目前采用准圆形波形。我们量化了残余轨道偏心率对 IMR 一致性测试的影响。我们发现，在 LIGO 频带内，偏心率为 $e_0 \gtrsim 0.1$ 的轨道偏心率（定义为 $10$ Hz）处的残余黑洞的最终推断质量和自旋中，偏心率会导致显着的系统偏差（对于总双星质量在 $65$-$200 \,M_{\odot}$ 范围内）。对于宇宙探索者 (CE) 观测到的双黑洞，系统偏差对于 $e_0 \gtrsim 0.015$（对于 $200$-$600 \,M_{\odot}$ 系统）变得显着。这种偏心引起的最终质量和自旋偏差导致 IMR 一致性测试中明显不一致，表现为对 GR 的错误违反。因此，波形模型的偏心校正对于构建稳健的伽马射线测试非常重要，特别是对于第三代探测器。我们还估计了对吸气参数与最终质量和最终旋转之间关系的偏心修正；它们被证明非常小。
The inspiral-merger-ringdown (IMR) consistency test checks the consistency of the final mass and final spin of a binary black hole merger remnant, independently inferred via the inspiral and merger-ringdown parts of the waveform. As binaries are expected to be nearly circularized when entering the frequency band of ground-based detectors, tests of general relativity (GR) currently employ quasicircular waveforms. We quantify the effect of residual orbital eccentricity on the IMR consistency test. We find that eccentricity causes a significant systematic bias in the inferred final mass and spin of the remnant black hole at an orbital eccentricity (defined at $10$ Hz) of $e_0 \gtrsim 0.1$ in the LIGO band (for a total binary mass in the range $65$-$200 \,M_{\odot}$). For binary black holes observed by Cosmic Explorer (CE), the systematic bias becomes significant for $e_0 \gtrsim 0.015$ (for $200$-$600 \,M_{\odot}$ systems). This eccentricity-induced bias on the final mass and spin leads to an apparent inconsistency in the IMR consistency test, manifesting as a false violation of GR. Hence, eccentric corrections to waveform models are important for constructing a robust test of GR, especially for third-generation detectors. We also estimate the eccentric corrections to the relationship between the inspiral parameters and the final mass and final spin; they are shown to be quite small.