The role of distant pulsars in the detectability of continuous gravitational waves
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Sternberg Astronomical Institute, Moscow State University（莫斯科国立大学斯特恩伯格天文研究所）；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）
Kathrin Grunthal, Nataliya Porayko, David J. Champion, Michael Kramer
备注：
11 pages, 9 figures, accepted for publication by A&A
One of the imminent science goals of pulsar timing arrays (PTAs) is the detection of a continuous gravitational wave (CGW) emitted by an individual supermassive black hole binary (SMBHB). SMBHBs that cause CGWs with GW frequencies $f_\mathrm{GW} > 10 \text{nHz}$ have undergone significant orbital evolution, hence a change of $f_\mathrm{GW}$ over time. In PTA data sets with sufficiently long observational time span, this means that the Earth and pulsar terms' contributions to the CGW signal signature can eventually become resolvable. Since the pulsar term is accumulated incoherently and thus often treated as an additional source of noise, this separation can prove to be beneficial for the detection of the CGW signal in the PTA data set. We aim to investigate to what extent resolvable Earth and pulsar terms affect currently used techniques for CGW searches with PTA data sets, that treat the pulsar term as an additional source noise. We focus on the dependency of the pulsar term frequencies on the pulsar's distance. We aim to answer the question of whether adding more distant pulsars to a PTA data set can mitigate biases and improve the detection of CGWs. We show that under ideal conditions, more distant pulsars can facilitate the CGW search with PTA data sets. Bayesian parameter estimation is yielding better parameter constraints and the frequentist per-frequentist optimal statistic search becomes more stable. However, using the realistic data set simulations, it was found that other configuration parameters of a PTA, such as the anisotropic distribution of pulsars and the effective number of pulsars in a PTA, can play a crucial role to the importance of this effect.
Resolving diffusion signatures in distant pulsar halos with current and future experiments
Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；University of Chinese Academy of Sciences（中国科学院大学）；TIANFU Cosmic Ray Research Center（天府宇宙线研究中心）
Magnetic-distortion-induced ellipticity and gravitational wave radiation of neutron stars: millisecond magnetars in short GRBs, Galactic pulsars, and magnetars
中子星由于磁畸变而可能产生非轴对称形变，是地基干涉测量探测器的连续引力波（GW）源。经过几十年的搜索，使用现有的GW探测器，没有证据表明GW信号来自任何脉冲星。椭圆率的上限越来越严格地限制在银河系的恒星上。在这项工作中，我们使用的椭圆率推断从假定的毫秒磁星在短伽马射线暴（SGRB），以估计其可探测性目前和未来的GW探测器。对于从SGRB数据推断的$\sim 1$ ms磁星，高级LIGO（aLIGO）和爱因斯坦望远镜（ET）的探测视界分别为$\sim 30$ Mpc和$\sim 600$ Mpc。利用SGRB毫秒磁星的椭圆率作为刻度，在假设椭圆率是磁畸变引起的情况下，我们估算了银河系中的毫秒磁星和磁星的椭圆率和引力波应变。我们发现，该结果与aLIGO O 1对银河系恒星和磁星的零探测结果是一致的。我们进一步预测，GW信号从这些恒星/磁星可能无法检测到目前设计的aLIGO探测器。ET检测器可能能够检测来自这些天线中的一些天线的一些相对低频的信号（$<50$ Hz）。受其设计灵敏度的限制，eLISA探测器似乎不适合探测来自银河系恒星和磁星的信号。
Search for Periodic Radio Signals from Double Neutron Star System Companions Using the Fast Folding Algorithm
College of Physics, Guizhou University（贵州大学物理学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Guizhou Radio Astronomical Observatory, Guizhou University（贵州大学贵州射电天文观测站）；College of Astronomy and Space Sciences, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Key Laboratory of Radio Astronomy, Chinese Academy of Sciences（中国科学院射电天文重点实验室）；International Centre of Supernovae, Yunnan Key Laboratory（云南 supernova 国际研究中心）
Multi-messenger Approaches to Supermassive Black Hole Binary Detection and Parameter Estimation: Implications for Nanohertz Gravitational Wave Searches with Pulsar Timing Arrays
Challenges in Binary Pulsar Timing Detection of Dark Matter Subhalos
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台暗物质与空间天文重点实验室）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Population synthesis of Galactic middle-aged pulsar wind nebulae I. Detection prospects for current and future instruments
Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚太空研究学院）；Institució Catalana de Recerca i Estudis Avançats (ICREA)（加泰罗尼亚高级研究学院）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Università degli Studi di Firenze（佛罗伦萨大学）；INFN - Sezione di Firenze（意大利国家核物理研究所佛罗伦萨分部）
Discovery of Hidden Extragalactic Pulsars in the Parkes Archival Data
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）；Center for Gravitation, Cosmology, and Astrophysics, Department of Physics and Astronomy, University of Wisconsin-Milwaukee（威斯康星大学密尔沃基分校物理与天文学系引力、宇宙学和天体物理学中心）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav)（澳大利亚研究理事会引力波发现卓越中心（OzGrav））；Department of Physics and Astronomy, Franklin and Marshall College（富兰克林和马歇尔学院物理与天文学系）；Department of Physics and Astronomy, West Virginia University（西弗吉尼亚大学物理与天文学系）；Center for Gravitational Waves and Cosmology, West Virginia University（西弗吉尼亚大学引力波与宇宙学中心）；School of Engineering, Murray State University（默里州立大学工程学院）
