From laboratory experiments to LISA Pathfinder: achieving LISA geodesic motion
F Antonucci, M Armano, H Audley, G Auger, M Benedetti, P Binetruy, C Boatella, J Bogenstahl, D Bortoluzzi, P Bosetti, N Brandt, M Caleno, A Cavalleri, M Cesa, M… 展开作者
F Antonucci, M Armano, H Audley, G Auger, M Benedetti, P Binetruy, C Boatella, J Bogenstahl, D Bortoluzzi, P Bosetti, N Brandt, M Caleno, A Cavalleri, M Cesa, M Chmeissani, G Ciani, A Conchillo, G Congedo, I Cristofolini, M Cruise, K Danzmann, F De Marchi, M Diaz-Aguilo, I Diepholz, G Dixon, R Dolesi, N Dunbar, J Fauste, L Ferraioli, D Fertin, W Fichter, E Fitzsimons, M Freschi, A García Marin, C García Marirrodriga, R Gerndt, L Gesa, D Giardini, F Gibert, C Grimani, A Grynagier, B Guillaume, F Guzmán, I Harrison, G Heinzel, M Hewitson, D Hollington, J Hough, D Hoyland, M Hueller, J Huesler, O Jeannin, O Jennrich, P Jetzer, B Johlander, C Killow, X Llamas, I Lloro, A Lobo, R Maarschalkerweerd, S Madden, D Mance, I Mateos, P W McNamara, J Mendestì, E Mitchell, A Monsky, D Nicolini, D Nicolodi, M Nofrarias, F Pedersen, M Perreur-Lloyd, A Perreca, E Plagnol, P Prat, G D Racca, B Rais, J Ramos-Castro, J Reiche, J A Romera Perez, D Robertson, H Rozemeijer, J Sanjuan, A Schleicher, M Schulte, D Shaul, L Stagnaro, S Strandmoe, F Steier, T J Sumner, A Taylor, D Texier, C Trenkel, D Tombolato, S Vitale, G Wanner, H Ward, S Waschke, P Wass, W J Weber, P Zweifel
备注：
Proceedings of the 8th LISA Symposium. To appear Class. Quantum Grav. 28 (2011)
This paper presents a quantitative assessment of the performance of the upcoming LISA Pathfinder geodesic explorer mission. The findings are based on the results of extensive ground testing and simulation campaigns using flight hardware and flight control and operations algorithms. The results show that, for the central experiment of measuring the stray differential acceleration between the LISA test masses, LISA Pathfinder will be able to verify the overall acceleration noise to within a factor two of the LISA requirement at 1 mHz and within a factor 6 at 0.1 mHz. We also discuss the key elements of the physical model of disturbances, coming from LISA Pathfinder and ground measurement, that will guarantee the LISA performance.
We present here results from the first-ever search for dark photon dark matter that could have coupled to baryons in LISA Pathfinder, the technology demonstrator for a space-based gravitational-wave antenna. After analyzing approximately three months of data taken by LISA Pathfinder in the frequency range $[2\times 10^{-5},5]$ Hz, corresponding to dark photon masses of $[8\times 10^{-20},2\times 10^{-14}]$ eV/$c^2$, we find no evidence of a dark-matter signal, and set upper limits on the strength of the dark photon/baryon coupling. To perform this search, we leveraged methods that search for q…
An important goal of the Laser Interferometer Space Antenna (LISA) is to observe a stochastic gravitational-wave background (SGWB). A study of possible correlated noise in LISA is relevant to establish limits for this future measurement. To test noise investigation methods under somewhat realistic conditions, we use the data of LISA Pathfinder (LPF). We calculate the coherence between the LPF differential acceleration of the two test-masses with magnetic fields, temperature, and micronewton cold gas thruster activity in the spacecraft. We apply our observed correlations to LISA, and estimate h…
Detection and characterization of instrumental transients in LISA Pathfinder and their projection to LISA
NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；IRFU, CEA, Université Paris-Saclay（法国原子能与替代能源研究所，法国原子能委员会，巴黎萨克雷大学）；ARTEMIS, Observatoire de la Côte d’Azur（阿尔特米斯计划，蔚蓝海岸天文台）；SYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE（时间-频率和光学生物物理实验室，巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学，法国计量院）；Department of Physics, University of Trento（特伦托大学物理系）；Department of Physics, Aristotle University of Thessaloniki（塞萨洛尼基亚里士多德大学物理系）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
Design of the magnetic diagnostics unit onboard LISA Pathfinder
LISA（Laser Interferometer Space Antenna）是欧空局和美国宇航局（NASA）的一项联合任务，旨在成为第一个星载引力波观测站。由于LISA将面临的高度复杂性和技术挑战，欧空局决定发射一个技术演示器，LISA探路者。LISA Pathfinder的有效载荷是所谓的LISA技术包，将是迄今为止飞行的最高灵敏度的测地探测器。LISA技术包设计用于测量标称自由降落（测地线运动）中两个试验质量之间的相对加速度。影响有效载荷的磁、热和辐射干扰由诊断子系统监测和处理。诊断子系统由几个模块组成，其中之一是磁诊断单元。其主要功能是评估由于磁效应引起的试验质量之间的差分加速度噪声。为此，它必须确定测试质量的磁特性，即它们的剩磁和磁化率。在本文中，我们将展示如何实现所需的精度。
We anticipate noise from the Laser Interferometer Space Antenna (LISA) will exhibit nonstationarities throughout the duration of its mission due to factors such as antenna repointing, cyclostationarities from spacecraft motion, and glitches as highlighted by LISA Pathfinder. In this paper, we use a surrogate data approach to test the stationarity of a time series which does not rely on the Gaussianity assumption. The main goal is to identify noise nonstationarities in the future LISA mission. This will be necessary for determining how often the LISA noise power spectral density (PSD) will need…
Building on the great success of the LISA Pathfinder mission, the outlines of a new LISA mission design were laid out at the $11^{\rm th}$ International LISA Symposium in Zurich. The revised design calls for three identical spacecraft forming an equilateral triangle with 2.5 million kilometer sides, and two laser links per side delivering full polarization sensitivity. With the demonstrated Pathfinder performance for the disturbance reduction system, and a well studied design for the laser metrology, it is anticipated that the new mission will have a sensitivity very close to the original LISA…
LISA Pathfinder（LPF）任务的主要目标是充分表征加速度噪声模型，并测试未来类似于eLISA概念的天基引力波观测站的关键技术。数据分析团队开发了LISA技术包（LTP）实验的复杂三维模型。这些模型用于模拟，但更重要的是，它们将用于飞行操作期间的参数估计目的。数据分析团队的任务之一是识别对仪器噪声特性有显著影响的物理效应。解决这个问题的一种方法是恢复拟合数据的LTP模型的基本参数。因此，我们希望定义一个最简单的模型，有效地解释观察结果。要做到这一点，采用贝叶斯框架，必须估计两个竞争模型之间的所谓贝叶斯因子。在我们的分析中，我们使用三种主要的不同方法来估计它：可逆跳马尔可夫链蒙特卡罗方法，施瓦茨准则和拉普拉斯近似。他们被施加到模拟LPF实验中，最可能的LTP模型，解释的意见是恢复。本文提出的同一类型的分析预计将在飞行操作中遵循。此外，上述方法的输出与实验设计的相关性进行了探索。
LISA Pathfinder (LPF) was a technology pioneering mission designed to test key technologies required for gravitational wave detection in space. In the low frequency regime (milli-Hertz and below), where space-based gravitational wave observatories will operate, temperature fluctuations play a crucial role since they can couple into the interferometric measurement and the test masses' free-fall accuracy in many ways. A dedicated temperature measurement subsystem, with noise levels in 10$\,μ$K$\,$Hz$^{-1/2}$ down to $1\,$mHz was part of the diagnostics unit on board LPF. In this paper we report …
The geosynchronous Laser Interferometer Space Antenna (gLISA) is a space-based gravitational wave (GW) mission that, for the past five years, has been under joint study at the Jet Propulsion Laboratory, Stanford University, the National Institute for Space Research (I.N.P.E., Brazil), and Space Systems Loral. If flown at the same time as the LISA mission, the two arrays will deliver a joint sensitivity that accounts for the best performance of both missions in their respective parts of the mHz band. This simultaneous operation will result in an optimally combined sensitivity curve that is "whi…
Gravitational Waves (GWs) were observed for the first time in 2015, one century after Einstein predicted their existence. There is now growing interest to extend the detection bandwidth to low frequency. The scientific potential of multi-frequency GW astronomy is enormous as it would enable to obtain a more complete picture of cosmic events and mechanisms. This is a unique and entirely new opportunity for the future of astronomy, the success of which depends upon the decisions being made on existing and new infrastructures. The prospect of combining observations from the future space-based ins…
The Laser Interferometer Space Antenna (LISA) will open the mHz frequency window of the gravitational wave (GW) landscape. Among all the new GW sources expected to emit in this frequency band, extreme mass-ratio inspirals (EMRIs) constitute a unique laboratory for astrophysics and fundamental physics. Here we show that EMRIs can also be used to extract relevant cosmological information, complementary to both electromagnetic (EM) and other GW observations. By using the loudest EMRIs (SNR$>$100) detected by LISA as dark standard sirens, statistically matching their sky localisation region with m…
The UV LED mission demonstrates the precise control of the potential of electrically isolated test masses that is essential for the operation of space accelerometers and drag free sensors. Accelerometers and drag free sensors were and remain at the core of geodesy, aeronomy, and precision navigation missions as well as gravitational science experiments and gravitational wave observatories. Charge management using photoelectrons generated by the 254 nm UV line of Hg was first demonstrated on Gravity Probe B and is presently part of the LISA Pathfinder technology demonstration. The UV LED missio…
