Search templates for gravitational waves from inspiraling binaries: Choice of template spacing.
Search templates for gravitational waves from inspiraling binaries: Choice of template spacing.
复制标题
搜索来自吸气双星的引力波模板：模板间距的选择。
DOI：
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发表时间：
1995
期刊：
影响因子：
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通讯作者：
B. Owen
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文献类型：
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作者：
B. Owen
人们早就知道，从激励双星中寻找引力波必须借助于信号处理方法，而匹配滤波技术最有可能用于探测激励“啁啾”。这意味着干涉仪的输出必须与许多波形模板交叉相关，以挖掘出隐藏在噪声中的微弱信号。模板具有几个参数的特征，这些参数在有限范围内连续变化；但是，由于用于执行搜索模板与输出的相互关联的计算能力是有限的，因此必须使用这些参数的某些离散值来选择实际使用的模板，这些参数的间隔是有限的。如果间距太小，则执行在线搜索所需的模板数量（以及计算能力）将变得令人望而却步；如果间距太大，许多啁啾将不会被检测到，因为它们的参数值离最近的模板的值太远。在本文中，我使用微分几何来扩展Sathyaprakash和Dhurandhar的早期形式，以估计模板间距，模板数量以及根据参数离散化损失的事件分数对单个干涉仪输出进行单次在线搜索所需的计算能力。我的公式只需要很少的数值计算就可以得到这些结果，并且对任意噪声谱和模板参数化都是有效的。我发现，最密集的合理搜索所需的计算能力是每秒几百千兆次浮点运算。到LIGO投入运行时，这将是可行的，但值得寻找减少这个数字的方法。
It has long been known that the search for gravitational waves from inspiraling binaries must be aided by signal processing methods, and that the technique of matched filtering is the most likely to be used for the detection of inspiral ``chirps'. This means that the output of an interferometer must be cross- correlated with many waveform templates to dig out faint signals buried in the noise. The templates are characterized by several parameters which vary continuously over some finite range; but because the amount of computing power available to perform the cross-correlations of the search templates with the output is finite, the actual templates used must be picked with certain discrete values of these parameters, which will have some finite spacing. If the spacing is too small, the number of templates (and therefore the computing power) needed to perform an on-line search becomes prohibitive; if the spacing is too large, many chirps will not be detected because the values of their parameters lie too far from those of the nearest template. In this paper I use differential geometry to extend the earlier formalism of Sathyaprakash and Dhurandhar to estimate the template spacing, number of templates, and computing power required for a single-pass, on-line search of the output of a single interferometer in terms of the fraction of events lost to parameter discretization. My formalism obtains these results with little numerical computation, and is valid for arbitrary noise spectra and template parameterizations. I find that the computing power needed for the most computationally intensive, reasonable search is of order several hundred Gigaflops. This will be feasible by the time LIGO is operational, but it is worth pursuing methods of reducing this number.