When searching for new gravitational-wave or electromagnetic sources, the $n$ signal parameters (masses, sky location, frequencies,...) are unknown. In practice, one hunts for signals at a discrete set of points in parameter space, with a computational cost that is proportional to the number of these points. If that is fixed, the question arises, where should the points be placed in parameter space? The current literature advocates selecting the set of points (called a "template bank") whose Wigner-Seitz (also called Voronoï) cells have the smallest covering radius ($\equiv$ smallest maximal mismatch). Mathematically, such a template bank is said to have "minimum thickness". Here, for realistic populations of signal sources, we compute the fraction of potential detections which are "lost" because the template bank is discrete. We show that at fixed computational cost, the minimum thickness template bank does not maximize the expected number of detections. Instead, the most detections are obtained for a bank which minimizes a particular functional of the mismatch. For closely spaced templates, the fraction of lost detections is proportional to a scale-invariant "quantizer constant" G, which measures the average squared distance from the nearest template, i.e., the average expected mismatch. This provides a straightforward way to characterize and compare the effectiveness of different template banks. The template bank which minimizes G is mathematically called the "optimal quantizer", and maximizes the expected number of detections. We review optimal quantizer and minimum thickness template banks that are built as n-dimensional lattices, showing that even the best of these offer only a marginal advantage over template banks based on the humble cubic lattice.
New approach to template banks of gravitational waves with higher harmonics: Reducing matched-filtering cost by over an order of magnitude
Institute for Advanced Study（高等研究院）；University of California at Santa Barbara（加州大学圣巴巴拉分校）；Tata Institute of Fundamental Research（塔塔基础研究院）；California Institute of Technology（加州理工学院）；Princeton University（普林斯顿大学）；Weizmann Institute of Science（魏茨曼科学研究所）
Semianalytic Sensitivity Estimates for Out-of-Bank Gravitational-Wave Signals
Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学理论天体物理研究所）；Department of Physics, University of Toronto（多伦多大学物理系）；David A. Dunlap Department of Astronomy, University of Toronto（多伦多大学大卫·A·邓普尔天文学系）
Assessing a Template-Based Approach for Core-Collapse Supernova Gravitational-Wave Detection
The Oskar Klein Centre, Department of Astronomy, Stockholm University（斯德哥尔摩大学天文学系奥斯卡·克莱因中心）；Department of Mathematics, University of Wisconsin–Madison（威斯康星大学麦迪逊分校数学系）
Enhancing online estimation of CBC parameters with the low-latency MBTA analysis
Université de Strasbourg, CNRS, IPHC UMR 7178（斯特拉斯堡大学）；Institut de Physique des 2 Infinis de Lyon (IP2I) - UMR 5822, Université de Lyon, Université Claude Bernard, CNRS（里昂大学）；Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3（萨瓦勃朗峰大学）；Università degli Studi di Urbino ’Carlo Bo’（乌尔比诺卡尔洛博大学）；INFN Sezione di Firenze（佛罗伦萨意大利国家核物理研究所）；Service de Physique Théorique, Université Libre de Bruxelles (ULB)（布鲁塞尔自由大学）
Neural Network Guided Parameter Space Constraints for Gravitational Wave Searches from Binary Black Holes
Institute of Advanced Research（高级研究所）；St.Xavier’s College (Autonomous)（圣泽维尔学院（自治））；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Nikhef（荷兰国家核与粒子物理研究所）；Centre for Development of Telematics (C-DOT)（电信发展中心）；Department of Physics, University of Massachusetts, Dartmouth（马萨诸塞大学达特茅斯分校物理系）
