In-depth analysis of LISA Pathfinder performance results: time evolution, noise projection, physical models, and implications for LISA
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 frequ...
| Autores: | , , , , , , , , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/417484 |
| Acceso en línea: | https://hdl.handle.net/2117/417484 https://dx.doi.org/10.1103/PhysRevD.110.042004 |
| Access Level: | acceso abierto |
| Palabra clave: | Gravitational wave detectors Gravitational wave Àrees temàtiques de la UPC::Enginyeria electrònica |
| Sumario: | 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 ¿¿1¿¿mHz, is consistent with the decaying pressure due to the outgassing of a single gaseous species. (2) Between ¿=36¿¿µ¿Hz and 1 mHz, the acceleration ASD shows a 1/¿ 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 ¿=18¿¿µ¿Hz, the ASD significantly deviates from the 1/¿ 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/¿ 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. |
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