The most powerful astrophysical events: Gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity
The most powerful astrophysical events: Gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity
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DOI：
10.1103/physrevd.96.024006
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发表时间：
2016-12
影响因子：
5
通讯作者：
D. Keitel;X. J. Forteza;S. Husa;L. London;A. Nagar;S. Bernuzzi;Enno Harms;M. Hannam;Sebastian Khan;M. Purrer;G. Pratten;V. Chaurasia
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作者：
D. Keitel;X. J. Forteza;S. Husa;L. London;A. Nagar;S. Bernuzzi;Enno Harms;M. Hannam;Sebastian Khan;M. Purrer;G. Pratten;V. Chaurasia
在短时间内，双黑洞（BBH）合并可能是可见宇宙中最强大的天体物理事件。在这里，我们基于数值相对论 (NR) 模拟和 X. Jimenez-Forteza 等人引入的分层拟合方法，提出了一个模型，该模型适合非进动准圆 BBH 系统的引力波峰值光度，作为组成黑洞的质量和自旋的函数。 [物理。修订版 D 95, 064024 (2017).PRVDAQ2470-001010.1103/PhysRevD.95.064024]。这种拟合在准确性和参数空间覆盖范围方面比以前的结果有所改进，并且可用于推断未来天体物理信号（如 GW150914 和 GW151226）峰值光度的后验分布。该模型已校准为 378 个非进动 NR 模拟的 l≤6 模式，质量比高达 18，无量纲自旋幅度高达 0.995，并包括不等自旋效应。我们还限制了对大质量比的微扰数值结果的拟合。对 NR 峰值光度不确定性的关键贡献的研究，例如 (i) 模式选择，(ii) 有限分辨率，(iii) 有限提取半径，以及 (iv) 将 NR 波形转换为光度的不同方法，使我们能够使用来自四种不同代码的 NR 模拟作为同质校准集。这项对组合 NR 和大质量比数据（包括更高模式）的系统拟合研究也为改进吸气-合并-振铃波形模型铺平了道路。
For a brief moment, a binary black hole (BBH) merger can be the most powerful astrophysical event in the visible Universe. Here we present a model fit for this gravitational-wave peak luminosity of nonprecessing quasicircular BBH systems as a function of the masses and spins of the component black holes, based on numerical relativity (NR) simulations and the hierarchical fitting approach introduced by X. Jimenez-Forteza et al. [Phys. Rev. D 95, 064024 (2017).PRVDAQ2470-001010.1103/PhysRevD.95.064024]. This fit improves over previous results in accuracy and parameter-space coverage and can be used to infer posterior distributions for the peak luminosity of future astrophysical signals like GW150914 and GW151226. The model is calibrated to the l≤6 modes of 378 nonprecessing NR simulations up to mass ratios of 18 and dimensionless spin magnitudes up to 0.995, and includes unequal-spin effects. We also constrain the fit to perturbative numerical results for large mass ratios. Studies of key contributions to the uncertainty in NR peak luminosities, such as (i) mode selection, (ii) finite resolution, (iii) finite extraction radius, and (iv) different methods for converting NR waveforms to luminosity, allow us to use NR simulations from four different codes as a homogeneous calibration set. This study of systematic fits to combined NR and large-mass-ratio data, including higher modes, also paves the way for improved inspiral-merger-ringdown waveform models.