Binary black hole spectroscopy
Binary black hole spectroscopy
复制标题
双黑洞光谱
DOI：
10.1088/0264-9381/24/5/005
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发表时间：
2006
影响因子：
3.5
通讯作者：
A. Sengupta
中科院分区：
文献类型：
--
作者：
C. Van Den Broeck;A. Sengupta
我们研究了自旋双星紧致物体的准圆形绝热吸进的后牛顿（PN）引力波参数估计。特别地，将幅度校正波形的性能与高级LIGO和EGO中更常用的受限波形进行了比较。在波形受限的情况下，源的特性只能从相位中提取。在幅度校正波形的情况下，频谱编码了丰富的附加信息，这导致参数估计的显着改进。在~ 100 Mpc的距离上，完整的PN波形可以高精度地提取总质量的参数，最高可达数百个太阳质量，而在有限的PN波形中，误差是质量的陡函数，准确的参数估计只能用于相对较轻的恒星质量双星。在低质量端，与受限制的波形相比，包含振幅修正的高级LIGO和EGO在合并时间上的误差分别减少了一个数量级和5倍；质量越高，这种差异就越大。单个分量的质量，很难用受限的波形来确定，如果使用幅度校正波形，就可以高精度地测量出来，在高级LIGO中误差低至百分之几，在EGO中误差低至百分之零点几。通常的自旋轨道参数β也很难用受限的波形来确定（EGO中的低质量系统除外），但是完整的波形给出的误差与符合Kerr界的最大可能值相比是很小的。这就提出了一种方法，可以找出一个或两个组件对象是否违反了这个界限。另一方面，我们发现自旋-自旋参数σ即使在使用完整波形时仍然难以确定。一般来说，所有的误差对自旋的大小和方向只有微弱的依赖性。我们还简要讨论了振幅修正对初始LIGO参数估计的影响。
We study parameter estimation with post-Newtonian (PN) gravitational waveforms for the quasi-circular, adiabatic inspiral of spinning binary compact objects. In particular, the performance of amplitude-corrected waveforms is compared with that of the more commonly used restricted waveforms, in Advanced LIGO and EGO. With restricted waveforms, the properties of the source can only be extracted from the phasing. In the case of amplitude-corrected waveforms, the spectrum encodes a wealth of additional information, which leads to dramatic improvements in parameter estimation. At distances of ∼100 Mpc, the full PN waveforms allow for high-accuracy parameter extraction for total mass up to several hundred solar masses, while with the restricted ones the errors are steep functions of mass, and accurate parameter estimation is only possible for relatively light stellar mass binaries. At the low-mass end, the inclusion of amplitude corrections reduces the error on the time of coalescence by an order of magnitude in Advanced LIGO and a factor of 5 in EGO compared to the restricted waveforms; at higher masses these differences are much larger. The individual component masses, which are very poorly determined with restricted waveforms, become measurable with high accuracy if amplitude-corrected waveforms are used, with errors as low as a few per cent in Advanced LIGO and a few tenths of a per cent in EGO. The usual spin–orbit parameter β is also poorly determined with restricted waveforms (except for low-mass systems in EGO), but the full waveforms give errors that are small compared to the largest possible value consistent with the Kerr bound. This suggests a way of finding out if one or both of the component objects violate this bound. On the other hand, we find that the spin–spin parameter σ remains poorly determined even when the full waveform is used. Generally, all errors have but a weak dependence on the magnitudes and orientations of the spins. We also briefly discuss the effect of amplitude corrections on parameter estimation in Initial LIGO.