Analysis and suppression of thermal effect of an ultra-stable laser interferometer for space-based gravitational waves detection

In this paper,we present a suppression method for the thermal drift of an ultra-stable laser interferometer.The detailed analysis on the Michelson interferometer indicates that the change in optical path length induced by temperature variation can be effectively reduced by choosing proper thickness and/or incident angle of a compensator.Taking the optical bench of the Laser Interferometer Space Antenna Pathfinder as an example,we analyze the optical bench model with a compensator and show that the temperature coefficient of this laser interferometer can be reduced down to 1 pm/K with an incident angle of 0.267828 rad.The method presented in this paper can be used in the design of ultra-stable laser interferometers,especially for space-based gravitational waves detection.

Fault diagnosis method of link control system for gravitational wave detection

To maintain the stability of the inter-satellite link for gravitational wave detection,an intelligent learning monitoring and fast warning method of the inter-satellite link control system failure is proposed.Different from the traditional fault diagnosis optimization algorithms,the fault intelligent learning method pro-posed in this paper is able to quickly identify the faults of inter-satellite link control system despite the existence of strong cou-pling nonlinearity.By constructing a two-layer learning network,the method enables efficient joint diagnosis of fault areas and fault parameters.The simulation results show that the average identification time of the system fault area and fault parameters is 0.27 s,and the fault diagnosis efficiency is improved by 99.8%compared with the traditional algorithm.

Sensitivity function analysis of gravitational wave detection with single-laser and large-momentum-transfer atomic sensors

Recently, a configuration using atomic interferometers （AIs） had been sug- gested for the detection of gravitational waves. A new AI with some additional laser pulses for implementing large momentum transfer was also put forward, in order to reduce the effect of shot noise and laser frequency noise. We use a sensitivity function to analyze all possible configurations of the new AI and to distinguish how many mo- menta are transferred in a specific configuration. By analyzing the new configuration, we further explore a detection scheme for gravitational waves, in particular, that ame- liorates laser frequency noise. We find that the amelioration occurs in such a scheme, but novelly, in some cases, the frequency noise can be canceled completely by using a proper data processing method.

Was LIGO’s Gravitational Wave Detection a False Alarm?

This article presents a new type of whitening filter (allowing the “passing” of some noise sources) applied to process the data recorded in LIGO’s GW150914 and GW151226 events. This new analysis shows that in the GW150914 event, the signals from the collision of two black holes are very similar to the 32.5 Hz noise sources observed in both of LIGO’s detectors. It also points out that these 32.5 Hz noise sources are powered by a 30 Hz sub harmonic, coming from the 60 Hz power system. In the GW1226 event, the same analysis points out that the NR template is very similar to the 120 Hz noise source. Therefore, the signals recorded in these events were probably generated by some small changes with the 60 Hz frequency in the US power grid. This can be caused, for example, by a power variation in the DC link, which can appear in both detectors in the same 10 ms time window. As this kind of power grid occurrence did not change the voltage levels, it may have gone unnoticed by LIGO’s electrical power supply’s monitoring system.

Gravitational Wave Detection Technology Development and Its Contribution to Cosmology

Gravitational wave detection has ushered in a new era of observing the universe, providing humanity with a novel window for cosmic cognition. This theoretical study systematically traces the developmental trajectory of gravitational wave detection technology and delves into its profound impact on cosmological research. From Einstein’s prediction in general relativity to LIGO’s groundbreaking discovery, the article meticulously delineates the key theoretical and technological milestones in gravitational wave detection, with particular emphasis on elucidating the principles and evolution of core detection technologies such as laser interferometers. The research thoroughly explores the theoretical application value of gravitational waves in verifying general relativity, studying the physics of compact celestial bodies like black holes and neutron stars, and precisely measuring cosmological parameters. The article postulates that gravitational wave observations may offer new research perspectives for addressing cosmological conundrums such as dark matter, dark energy, and early universe evolution. The study also discusses the scientific prospects of combining gravitational wave observations with electromagnetic waves, neutrinos, and other multi-messenger observations, analyzing the potential value of this multi-messenger astronomy in deepening cosmic cognition. Looking ahead, the article examines cutting-edge concepts such as space-based gravitational wave detectors and predicts potential developmental directions for gravitational wave astronomy. This research not only elucidates the theoretical foundations of gravitational wave detection technology but also provides a comprehensive theoretical framework for understanding the far-reaching impact of gravitational waves on modern cosmology.

Data Analysis Methods and Signal Processing Techniques in Gravitational Wave Detection

Gravitational wave detection is one of the most cutting-edge research areas in modern physics, with its success relying on advanced data analysis and signal processing techniques. This study provides a comprehensive review of data analysis methods and signal processing techniques in gravitational wave detection. The research begins by introducing the characteristics of gravitational wave signals and the challenges faced in their detection, such as extremely low signal-to-noise ratios and complex noise backgrounds. It then systematically analyzes the application of time-frequency analysis methods in extracting transient gravitational wave signals, including wavelet transforms and Hilbert-Huang transforms. The study focuses on discussing the crucial role of matched filtering techniques in improving signal detection sensitivity and explores strategies for template bank optimization. Additionally, the research evaluates the potential of machine learning algorithms, especially deep learning networks, in rapidly identifying and classifying gravitational wave events. The study also analyzes the application of Bayesian inference methods in parameter estimation and model selection, as well as their advantages in handling uncertainties. However, the research also points out the challenges faced by current technologies, such as dealing with non-Gaussian noise and improving computational efficiency. To address these issues, the study proposes a hybrid analysis framework combining physical models and data-driven methods. Finally, the research looks ahead to the potential applications of quantum computing in future gravitational wave data analysis. This study provides a comprehensive theoretical foundation for the optimization and innovation of gravitational wave data analysis methods, contributing to the advancement of gravitational wave astronomy.

Multifrequency Gravitational Wave Background from Continuous Sources

Gravitational waves have been detected in the past few years from several transient events such as merging stellar mass black holes, binary neutron stars, etc. These waves have frequencies in a band ranging from a few hundred hertz to around a kilohertz to which LIGO type instruments are sensitive. LISA would be sensitive to much lower range of frequencies from SMBH mergers. Apart from these cataclysmic burst events, there are innumerable sources of radiation which are continuously emitting gravitational waves of all frequencies. These include a whole mass range of compact binary and isolated compact objects as well as close planetary stellar entities. In this work, quantitative estimates are made of the gravitational wave background produced in typical frequency ranges from such sources emitting over a Hubble time and the fluctuations in the h values measured in the usual devices. Also estimates are made of the high frequency thermal background gravitational radiation from hot stellar interiors and newly formed compact objects.

Advancing space-based gravitational wave astronomy: Rapid parameter estimation via normalizing flows

Gravitational wave(GW) astronomy is witnessing a transformative shift from terrestrial to space-based detection, with missions like Taiji at the forefront. While the transition brings unprecedented opportunities for exploring massive black hole binaries(MBHBs), it also imposes complex challenges in data analysis, particularly in parameter estimation amidst confusion noise.Addressing this gap, we utilize scalable normalizing flow models to achieve rapid and accurate inference within the Taiji environment. Innovatively, our approach simplifies the data's complexity, employs a transformation mapping to overcome the year-period time-dependent response function, and unveils additional multimodality in the arrival time parameter. Our method estimates MBHBs several orders of magnitude faster than conventional techniques, maintaining high accuracy even in complex backgrounds. These findings significantly enhance the efficiency of GW data analysis, paving the way for rapid detection and alerting systems and enriching our ability to explore the universe through space-based GW observation.

Applying deep neural networks to the detection and space parameter estimation of compact binary coalescence with a network of gravitational wave detectors

In this paper, we study an application of deep learning to the advanced laser interferometer gravitational wave observatory(LIGO)and advanced Virgo coincident detection of gravitational waves(GWs) from compact binary star mergers. This deep learning method is an extension of the Deep Filtering method used by George and Huerta(2017) for multi-inputs of network detectors.Simulated coincident time series data sets in advanced LIGO and advanced Virgo detectors are analyzed for estimating source luminosity distance and sky location. As a classifier, our deep neural network(DNN) can effectively recognize the presence of GW signals when the optimal signal-to-noise ratio(SNR) of network detectors ≥ 9. As a predictor, it can also effectively estimate the corresponding source space parameters, including the luminosity distance D, right ascension α, and declination δ of the compact binary star mergers. When the SNR of the network detectors is greater than 8, their relative errors are all less than 23%.Our results demonstrate that Deep Filtering can process coincident GW time series inputs and perform effective classification and multiple space parameter estimation. Furthermore, we compare the results obtained from one, two, and three network detectors;these results reveal that a larger number of network detectors results in a better source location.

Numerical simulations of the wavefront distortion of inter-spacecraft laser beams caused by solar wind and magnetospheric plasmas

Plasma turbulence may lead to additional wavefront distortion of inter-spacecraft laser beams during the operation of spaceborne gravitational wave(GW)observatories,e.g.Tian Qin.By making use of the Space Weather Modelling Framework(SWMF)model and realistic orbit data for the Tian Qin constellation,the characteristic parameters of the plasma turbulence present at the Tian Qin orbit are obtained.As a first step,this work is based on the assumptions that the cold plasma approximation is valid and that the effects of the electromagnetic field induced by charge separation within the Debye length on the laser's wavefront can be ignored.An atmospheric turbulence-laser interaction model is then applied to analyze the effects of the plasma turbulence on the inter-spacecraft laser's wavefront.The preliminary results show that the wavefront distortion caused by the plasma turbulence is 10^-9 rad,which is significantly less than the designated error budget,i.e.10^-6 rad,and thus will not affect the laser interferometry.

高水平应用型大学“检测技术”课程教学探索与实践——以北京信息科技大学为例

构筑全环境立德树人“大思政”格局,是全面提升高水平应用型大学教育教学质量的关键所在。“检测技术”是电子信息大类专业特色主干课程,其教学内容与仪器领域科技前沿紧密结合,具有高度的学科交叉特性。融合思政元素开展教学工作具有独特的优势,是新时代教育教学改革的必然趋势。以北京信息科技大学“检测技术”课程为例,探索了以课程教学为主线、科技前沿技术服务课程思政的教学模式,在教学实例方面,从激光干涉产生的“小”条纹入手,引导学生关注知识点背后隐藏的“大”学问,启发学生见“微”知“著”,树立精益求精的科学态度,坚定科技报国的理想。

空间引力波探测干涉仪探测模式比较研究

为了实现毫赫兹频段的引力波信号测量,基于激光干涉体制的空间引力波探测计划要求干涉系统硬件本底噪声低于星间散粒噪声极限,这对光机设计及相应干涉载荷提出了严苛的工程指标。本文从探测模式选择的角度出发,推导了在单探测器模式和平衡模式下读出噪声和杂散光噪声在干涉信号中的表达形式,并就科学干涉仪的弱光干涉过程进行了详细讨论。结果表明,平衡模式可以跨量级的抑制激光功率涨落和后向杂散光引起的干涉相位噪声,但其抑制能力受限于合束器的不等比分光性质。为此引入相对增益因子来补偿合束器的不等比分光特性,进一步的分析表明,电子学手段的增益补偿只能消除不等比分光对两者之一的影响,不能同时兼顾,需要在激光功率涨落噪声和杂散光噪声的抑制之间平衡选择增益补偿。即便如此,平衡模式下的跨量级的噪声抑制能力,仍然可望降低对激光功率涨落和望远镜杂散光的工程指标要求。

超长空间激光传输数值模拟研究进展

文章主要围绕空间引力波探测中超长空间链路传输部分进行介绍,概述了目前国内外星间传输仿真时采用的计算方法,以及指向抖动引起的相位噪声分析方法。相较于地基引力波探测,空间引力波探测可以有效降低噪声,增加干涉臂长度,从而实现更高精度、更低频率的探测。在长达数百万公里的传输距离,以及皮米量级数值模拟的精度要求下,需要考虑指向角变化引起的相位噪声。研究表明,在2.5×10~9 m的传输距离下,离焦和像散是影响指向抖动噪声的主要像差。通常情况下,相位驻点位置与原点位置存在一定偏离,需要对望远镜角度进行调整,才能使相位噪声最小化。在相位驻点位置进行引力波探测,可以有效降低相位噪声,并降低望远镜出瞳波前的质量要求。而大的离焦像差与小的彗差可以使相位驻点接近光轴,提高接收到的激光功率。

空间引力波星载望远镜测试与评估技术研究进展

在空间引力波探测任务中,星载望远镜承担太空超长干涉光路双向光束准直的重要作用。空间引力波探测对星载望远镜提出了pm级光程稳定性和低于10^(-10)级后向杂散光水平的极高要求。超高水平指标要求超过了当前测试技术的精度极限,因此,针对星载望远镜发展测试与评估技术并开展系统超高精度测试是空间引力波探测计划成功的重要前提。本文在概述国内外在研的空间引力波探测星载望远镜研制情况的基础上,重点围绕星载望远镜的核心技术指标——光程稳定性和后向杂散光,介绍了在研望远镜的测试技术发展现状和已经取得的部分测试成果,以及各研究单位进一步的测试计划,为我国的空间引力波探测的星载望远镜测试与评估技术发展提供参考。

星载望远镜消光材料积分散射特性测试研究(英文)

在散射理论的基础上,介绍了一种星载望远镜消光材料积分散射特性测试装置,实现对星载望远镜消光材料散射特性更为全面的测量。对积分散射理论、系统构造、系统性能进行了阐述。对系统进行建模仿真分析,得到结论:消光材料的散射特性在不同点位和入射角下存在明显差异,系统能够测量多种条件下消光材料的散射特性,并得到消光材料全面的散射特性分布。研究结果为根据消光材料特性进行针对性设计提供了更全面、更准确的散射特性分布,为杂散光的测量与抑制、高性能光学仪器的研制与装调以及计算光学等领域的研究提供了参考。为空间引力波探测星载望远镜系统的材料选型、特性研究、杂散光分析与抑制提供了基础。

基于FEM的引力参考传感器自引力计算与补偿

空间引力波探测太极计划将利用激光干涉的方法,测量两个检验质量之间的距离变化反演引力波信息。在0.1 mHz处,要求检验质量在敏感轴方向的总残余加速度保持在3×10^(-15)m·s^(-2)/√Hz以下。由航天器载荷静引力、热形变和质量波动引起的自引力噪声是检验质量的残余加速度噪声主要来源之一,要求检验质量在敏感轴方向的自引力加速度小于1×10^(-10)m/s^(2),引力梯度小于5×10^(-8)s^(-2)。为了计算检验质量处的自引力大小和引力梯度,针对检验质量与引力源几何形状的不规则性,基于有限元法编写程序计算了引力参考传感器中的引力源作用在检验质量上的线加速度、角加速度和引力梯度。为了缩短计算时间,提出“类自适应”网格划分方法以减小网格数量,并设计了配重以补偿自引力。计算结果显示,经过补偿后的检验质量在敏感轴方向的自引力加速度为9.2377×10^(-12)m/s^(2),引力梯度为-2.5691×10^(-8)s^(-2),满足设计要求。本研究能够为航天器和引力参考传感器的设计与引力补偿提供参考与指导。

空间引力波探测星载望远镜专题导读(二)

探测空间引力波有望揭开更多的宇宙奥秘。在国家重点研发计划项目的支持下,《光电工程》组织了“空间引力波探测星载望远镜专题(二)”。专题围绕空间引力波探测星载望远镜设计与分析、建造与装调、测试与评估等几个方面介绍了近期的主要研究进展,将为相关领域学者和专家提供技术研究的参考和合作交流的平台,并将积极推动我国空间引力波探测计划的研究进程。

空间应用激光薄膜元件研究进展

随着空间激光技术的不断进步,空间激光系统逐渐向更短应用波长、更长使用寿命、更高应用轨道等方向发展,对薄膜元件提出了更高的性能要求。本文综述国内外主要空间激光器的发展方向,在空间激光系统研制过程中薄膜元件的真空、高低温、质子辐射、伽马射线辐射等空间环境损伤效应,以及使役条件(即空间与激光耦合作用)下薄膜的性能演化机理。介绍在高性能空间激光薄膜元件研制技术方面的新进展,结合空间引力波探测、深空探测等未来发展方向对空间激光薄膜元件提出了展望。

地基引力波探测激光干涉仪的真空残余气体噪声分析

引力波是时空弯曲产生的涟漪波动.引力波探测对促进人类认识自然和科学技术进步均具有深远意义.由于引力波信号非常微弱,地基引力波探测器需要超高真空环境来保证激光干涉仪的稳定运行.本文阐述了残余气体噪声对地基引力波探测装置灵敏度的影响,并从第三代地基引力波探测原型机和全尺寸装置的真空系统设计出发,通过理论分析和模拟,给出真空系统压强、环境温度、残余气体质量和种类、测试质量的曲率半径等因素对引力波探测灵敏度的影响.这为引力波探测原型机和全尺寸装置的真空系统设计和建设提供了重要的理论依据.

基于MBSE的空间引力波探测系统指标管理及其探测灵敏度分析

为了将空间引力波探测系统论证过程中顶层指标分解与系统级性能分析过程动态关联,提供对空间科学任务全生命周期信息的管理与应用分析能力,提出了基于模型的系统工程(MBSE)的空间引力波探测系统指标管理及其探测灵敏度分析方法。通过系统建模语言(SysML)构建空间引力波探测系统指标参数模型,并解析模型内容,筛选和记录指标参数,最后,通过探测灵敏度这一评价空间引力波探测系统探测能力的主要标准,实现空间引力波探测系统对不同科学目标的探测性能分析。结果表明,该方法可统一管理和追溯所有指标内容,为空间引力波探测系统顶层指标论证和系统级性能评价提供了支持。