In-depth analysis of LISA Pathfinder performance results

Time evolution, noise projection, physical models, and implications for LISA

authored by

LISA Pathfinder Collaboration , M. Armano, H. Audley, J. Baird, P. Binetruy, M. Born, D. Bortoluzzi, E. Castelli, A. Cavalleri, A. Cesarini, V. Chiavegato, A. M. Cruise, D. Dal Bosco, K. Danzmann, M. De Deus Silva, I. Diepholz, G. Dixon, R. Dolesi, L. Ferraioli, V. Ferroni, E. D. Fitzsimons, M. Freschi, L. Gesa, D. Giardini, F. Gibert, R. Giusteri, C. Grimani, J. Grzymisch, I. Harrison, M. S. Hartig, G. Heinzel, M. Hewitson, D. Hollington, D. Hoyland, M. Hueller, H. Inchauspé, O. Jennrich, P. Jetzer, B. Johlander, N. Karnesis, B. Kaune, N. Korsakova, C. J. Killow, J. A. Lobo, J. P. López-Zaragoza, R. Maarschalkerweerd, D. Mance, V. Martín, L. Martin-Polo, F. Martin-Porqueras, G. Wanner

Abstract

We present an in-depth analysis of the LISA Pathfinder differential acceleration performance over the entire course of its science operations, spanning approximately 500 days. We find: (1) The evolution of the Brownian noise that dominates the acceleration amplitude spectral density (ASD), for frequencies f≳1 mHz, is consistent with the decaying pressure due to the outgassing of a single gaseous species. (2) Between f=36 μHz and 1 mHz, the acceleration ASD shows a 1/f tail in excess of the Brownian noise of almost constant amplitude, with ≃20% fluctuations over a period of a few days, with no particular time pattern over the course of the mission. (3) At the lowest considered frequency of f=18 μHz, the ASD significantly deviates from the 1/f behavior, because of temperature fluctuations that appear to modulate a quasistatic pressure gradient, sustained by the asymmetries of the outgassing pattern. We also present the results of a projection of the observed acceleration noise on the potential sources for which we had either a direct correlation measurement or a quantitative estimate from dedicated experiments. These sources account for approximately 40% of the noise power in the 1/f tail. Finally, we analyze the possible sources of the remaining unexplained fraction and identify the possible measures that may be taken to keep those under control in LISA.

Organisation(s)

Institute of Gravitation Physics
PhoenixD: Photonics, Optics, and Engineering - Innovation Across Disciplines
Institute of Quantum Optics

External Organisation(s)

European Space Astronomy Centre
European Space Research and Technology Centre (ESTEC)
AGH University of Science and Technology (AGH UST)
Observatoire de Paris (OBSPARIS)
Université Paris-Saclay
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
University of Trento
Istituto Nazionale di Fisica Nucleare (INFN)
NASA Goddard Space Flight Center (NASA-GSFC)
Fondazione Bruno Kessler
University of Urbino "Carlo Bo"
University of Birmingham
ETH Zurich
Royal Observatory
Autonomous University of Barcelona (UAB)
Institute of Space Studies of Catalonia (IEEC)
Qioptiq Photonics GmbH and Co.KG
isardSAT
European Space Operation Center (ESOC)
Imperial College London
Heidelberg University
Universität Zürich (UZH)
Aristotle University of Thessaloniki (A.U.Th.)
University of Glasgow

Type

Article

Journal

Physical Review D

Volume

110

ISSN

2470-0010

Publication date

21.08.2024

Publication status

Published

Peer reviewed

Yes

ASJC Scopus subject areas

Nuclear and High Energy Physics

Electronic version(s)

https://doi.org/10.1103/PhysRevD.110.042004 (Access: Closed)
https://doi.org/10.48550/arXiv.2405.05207 (Access: Open)