In previous work [1], three TAIJI orbital deployments have been proposed to compose alternative LISA-TAIJI networks, TAIJIm (leading the Earth by $20^\circ$ and $-60^\circ$ inclined with respect to ecliptic plane), TAIJIp (leading the Earth by $20^\circ$ and $+60^\circ$ inclined), TAIJIc (colocated and coplanar with LISA) with respect to the LISA mission (trailing the Earth by $20^\circ$ and $+60^\circ$ inclined). And the LISA-TAIJIm network has been identified as the most capable configuration for massive black hole binary observation. In this work, we examine the performance of three networks to the stochastic gravitational wave background (SGWB) especially for the comparison of two eligible configurations, LISA-TAIJIm and LISA-TAIJIp. This investigation shows that the detectability of LISA-TAIJIm is competitive with the LISA-TAIJIp network for some specific SGWB spectral shapes. And the capability of LISA-TAIJIm is also identical to LISA-TAIJIp to separate the SGWB components by determining the parameters of signals. Considering the performances on SGWB and massive black hole binaries observations, the TAIJIm could be recognized as an optimal option to fulfill joint observations with LISA.
Alternative LISA-TAIJI networks: polarization separation of the stochastic gravitational wave background
Institute of Fundamental Physics and Quantum Technology, Ningbo University(宁波大学基础物理与量子技术研究院);Department of Physics, School of Physical Science and Technology, Ningbo University(宁波大学物理科学与技术学院);Department of Physics, Faculty of Arts and Sciences, Beijing Normal University(北京师范大学艺术与科学学院物理系)
Overlap reduction functions for a polarized stochastic gravitational-wave background in the Einstein Telescope-Cosmic Explorer and the LISA-Taiji networks
本文将基于球谐展开的重叠减少函数计算方法推广到第三代地基 Einstein Telescope-Cosmic Explorer 网络及 LISA-Taiji 空间联合任务,以分析极化随机引力波背景。
PTA-Compatible Domain Walls at LISA and Taiji: Bayesian Reconstruction and Multiband Inference
Nanjing Normal University(南京师范大学);Scuola Superiore Meridionale, Università degli studi di Napoli “Federico II”(那不勒斯费德里科二世大学南方高等学院);INFN - Sezione di Napoli(意大利国家核物理研究所那不勒斯分部)
Correlated Galactic Confusion Foreground for the LISA-Taiji-TianQin Network and Its Impacts on Resolvable-Source Analysis
Institute of Mechanics, Chinese Academy of Sciences(中国科学院力学研究所);University of Chinese Academy of Sciences (UCAS)(中国科学院大学);Hangzhou Institute for Advanced Study, UCAS(杭州高等研究院,中国科学院大学);Lanzhou University(兰州大学)
Construction of Sensitivity Curves for Dynamic LISA and Taiji
School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS)(中国科学院大学天文与空间科学学院);School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS(中国科学院大学杭州高等研究院基础物理与数学学院);International Centre for Theoretical Physics Asia-Pacific, UCAS(中国科学院大学亚太理论物理中心)
Subtraction of the confusion foreground and parameter uncertainty of resolvable galactic binaries on the networks of space-based gravitational-wave detectors
Testing the Transverse Scalar Mode of Gravitational Quantum Field Theory with Taiji and LISA
Hangzhou Institute for Advanced Study, UCAS(杭州高等研究院);Institute of Theoretical Physics, Chinese Academy of Sciences(中国科学院理论物理研究所);University of Chinese Academy of Sciences(中国科学院大学);International Centre for Theoretical Physics Asia-Pacific, UCAS(亚太理论物理中心);Taiji Laboratory for GW Universe (Beijing/Hangzhou), University of Chinese Academy of Sciences(太极引力波宇宙实验室)
Identifying Monochromatic Signals in LISA and Taiji via Spectral Split: Gravitational Waves versus Ultralight Dark Matter
University of Chinese Academy of Sciences (UCAS)(中国科学院大学);Hangzhou Institute for Advanced Study, UCAS(杭州高等研究院,中国科学院大学);Institute of Theoretical Physics, Chinese Academy of Sciences(中国科学院理论物理研究所);International Center for Theoretical Physics Asia-Pacific(亚太理论物理中心);School of Astronomy and Space Science, UCAS(天文学与空间科学学院,中国科学院大学)
Detectability of Gravitational-Wave Memory with LISA: A Bayesian Approach
CEA(法国原子能和替代能源委员会);Université Paris-Saclay(巴黎萨克雷大学);Centre national d’études spatiales (CNES)(法国国家空间研究中心);CERN(欧洲核子研究组织);Institut de Física d’Altes Energies (IFAE)(高能物理研究所);The Barcelona Institute of Science and Technology(巴塞罗那科学技术研究院);Niels Bohr Institute(尼尔斯·玻尔研究所);KU Leuven(荷语鲁汶大学);Leuven Gravity Institute(鲁汶引力研究所);SISSA(国际高等研究院);INFN Sezione di Trieste(意大利国家核物理研究所的里雅斯特分部);IFPU - Institute for Fundamental Physics of the Universe(宇宙基础物理研究所)
Distinguishing Monochromatic Signals in LISA and Taiji: Ultralight Dark Matter versus Gravitational Waves
School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS(杭州高等研究院基础物理与数学学院);Institute of Theoretical Physics, Chinese Academy of Sciences(中国科学院理论物理研究所);University of Chinese Academy of Sciences (UCAS)(中国科学院大学);International Center for Theoretical Physics Asia-Pacific(亚太理论物理中心)
Testing Gravitational-Wave Signal From Verification Binaries with Space-Based Gravitational-Wave Detectors
School of Science, Shenzhen Campus of Sun Yat-sen University(中山大学深圳校区理学院);School of Electrical and Electronic Engineering, Anhui Science and Technology University(安徽科技学院电气与电子工程学院)
Constraints and detection capabilities of GW polarizations with space-based detectors in different TDI combinations
College of Physics, Chongqing University(重庆大学物理学院);Department of Physics and Chongqing Key Laboratory for Strongly Coupled Physics, Chongqing University(重庆大学物理系及强耦合物理重庆市重点实验室)
Calibration Method of Spacecraft-Inertial Sensor Center-of-Mass Offset for the Taiji Gravitational Wave Detection Mission under Science Mode
State Key Laboratory of Micro-Spacecraft Rapid Design and Intelligent Cluster, Harbin Institute of Technology(哈尔滨工业大学微纳航天器快速设计与智能集群全国重点实验室);Center for Gravitational Wave Experiment, Institute of Mechanics, Chinese Academy of Sciences(中国科学院力学研究所引力波实验中心);Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences(中国科学院大学杭州高等研究院);Lanzhou Center of Theoretical Physics, Lanzhou University(兰州大学理论物理研究中心);National Space Science Center, Chinese Academy of Sciences(中国科学院国家空间科学中心)
Probing non-Gaussianity during reheating with SIGW in the LISA band
Keemilise ja Bioloogilise Füüsika Instituut(化学与生物物理研究所);Institute for Theoretical Physics, Leibniz University Hannover(汉诺威莱布尼茨大学理论物理研究所);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)
Gravitational waves from bodies orbiting the Galactic Center black hole and their detectability by LISA
我们提出了第一个完全相对论性的研究引力辐射的机构在圆形赤道轨道周围的大规模黑洞在银河系中心,Sgr A *,我们评估各种物体的引力波探测器LISA的可探测性。我们的计算是基于克尔时空的微扰理论,并考虑到在克尔度规潮汐力引起的罗氏极限。在LISA检测器的信噪比,以及在LISA波段所花费的时间,进行了评估。我们在黑洞扰动工具包框架内的开源SageMath包中实现了所有计算工具。我们发现白矮星,中子星,恒星黑洞,质量大于$10^{-4} M_\odot$的原始黑洞,质量低于$\sim 2.5\, M_\odot$的主序星和围绕Sgr A * 运行的棕矮星,在LISA数据的一年中都可以被探测到,并且在至少$10^5$年的时间里,在缓慢的螺旋形轨道上,或者在最内侧的稳定圆形轨道上,信噪比大于10(紧凑型天体)或罗氏极限(主序星和褐矮星)。最长的带内时间,$10^6$年的顺序,实现了原始黑洞的质量$\sim 10^{-3} M_\odot$到$10^{-5} M_\odot$,取决于自旋的Sgr A *,以及褐矮星,其次是白矮星和低质量的主序星。这些物体的长时间带内使Sgr A * 成为LISA的有价值的目标。我们还考虑了在附近星系M32的核中的大质量黑洞周围的近圆形轨道上的天体,发现其中,致密天体和褐矮星在LISA波段停留$10^3$至$10^4$年,1年信噪比大于10。
Populations of double white dwarfs in Milky Way satellites and their detectability with LISA
银河系矮卫星是编码早期结构形成的独特物体,因此代表了进入高红移宇宙的窗口。到目前为止,他们的研究仅使用电磁波进行。未来的激光干涉仪空间天线(LISA)有可能在双白矮星(DWD)双星发射的引力波中揭示银河系卫星。我们调查的引力波(GW)信号可检测的LISA作为一种可能的工具,用于识别和表征的银河系卫星。我们使用的二进制人口合成技术来模拟人口的DWDs在矮卫星,我们评估的LISA检测的数量的影响时,改变恒星的总质量,距离,恒星形成的历史和金属丰度的卫星。我们校准预测已知的银河系卫星观测到的属性。我们发现,DWDs发射频率$\gtrsim 3\,$兆赫可以检测到银河系卫星在大银河系的距离。这些高频DWD每个卫星的数量主要取决于它的质量,距离,年龄和恒星形成的历史,只有轻微的依赖于其他假设,如金属丰度的演变。我们发现,矮星系与$M_\star>10^6\,$ M $_{\odot}$可以主机可检测的LISA源的数量,与卫星的质量成线性比例的检测。我们预测,在已知的卫星中,人马座,天炉座,雕塑家和麦哲伦云可以用LISA探测到。作为一个不会受到污染和尘埃灭绝的全天空调查,LISA将提供对银河系和矮卫星星系的观测,这些星系对银河系考古学和近场宇宙学很有价值。