An algorithm is proposed for constructing a group (ensemble) pulsar time based on the application of optimal Wiener filters. This algorithm makes it possible to separate the contributions of variations of the atomic time scale and of the pulsar rotation to barycentric residual deviations of the pulse arrival times. The method is applied to observations of the pulsars PSR B1855+09 and PSR B1937+21, and is used to obtain corrections to UTC relative to the group pulsar time PT$_{\rm ens}$. Direct comparison of the terrestrial time TT(BIPM06) and the group pulsar time PT$_{\rm ens}$ shows that they disagree by no more than $0.4\pm 0.17\; μ$s. Based on the fractional instability of the time difference TT(BIPM06) -- PT$_{\rm ens}$, a new limit for the energy density of the gravitational-wave background is established at the level $Ω_g {h}^2\sim 10^{-9}$.
Noise-marginalized optimal statistic: A robust hybrid frequentist-Bayesian statistic for the stochastic gravitational-wave background in pulsar timing arrays
Not just a phase: detecting nanohertz gravitational waves from phase alone
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Monash University（莫纳什大学）；OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery（引力波发现ARC卓越中心）；Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）
Scalable continuous gravitational wave detection in PTA data with non-parametric red noise suppression and optimal pulsar selection
National Gravitation Laboratory, MOE Key Laboratory of Fundamental Physical Quantities Measurements, Department of Astronomy and School of Physics, Huazhong University of Science and Technology（华中科技大学天文系与物理学院）；The University of Texas Rio Grande Valley（德克萨斯大学里奥格兰德河谷分校）；IIT Hyderabad（印度理工学院海德拉巴分校）；State Key Laboratory of Radio Astronomy and Technology, Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
Optimal Pulsar Timing Array Strategies with the Deep Synoptic Array
New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院）；National Radio Astronomy Observatory（国家射电天文台）；Oregon State University（俄勒冈州立大学）；Green Bank Observatory（格林班克天文台）；SETI Institute（SETI研究所）；University of Wisconsin-Milwaukee（威斯康星大学密尔沃基分校）；University of North Carolina, Chapel Hill（北卡罗来纳大学教堂山分校）；Newcastle University（纽卡斯尔大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Widener University（韦德纳大学）；Lafayette College（拉斐特学院）；Institute for Gravitational Wave Astr（引力波天体物理研究所）
A Joint Optimal Search for Gravitational Waves from Resolved and Unresolved Supermassive Binary Black Holes with Pulsar Timing Arrays
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；School of Natural Sciences, Institute for Advanced Study（普林斯顿高等研究院自然科学学院）
