论文标题

etpathfinder:干涉重力波检测器的低温测试床

ETpathfinder: a cryogenic testbed for interferometric gravitational-wave detectors

论文作者

Utina, A., Amato, A., Arends, J., Arina, C., de Baar, M., Baars, M., Baer, P., van Bakel, N., Beaumont, W., Bertolini, A., van Beuzekom, M., Biersteker, S., Binetti, A., ter Brake, H. J. M., Bruno, G., Bryant, J., Bulten, H. J., Busch, L., Cebeci, P., Collette, C., Cooper, S., Cornelissen, R., Cuijpers, P., van Dael, M., Danilishin, S., Dixit, D., van Doesburg, S., Doets, M., Elsinga, R., Erends, V., van Erps, J., Freise, A., Frenaij, H., Garcia, R., Giesberts, M., Grohmann, S., Van Haevermaet, H., Heijnen, S., van Heijningen, J. V., Hennes, E., Hennig, J. -S., Hennig, M., Hertog, T., Hild, S., Hoffmann, H. -D., Hoft, G., Hopman, M., Hoyland, D., Iandolo, G. A., Ietswaard, C., Jamshidi, R., Jansweijer, P., Jones, A., Jones, P., Knust, N., Koekoek, G., Koroveshi, X., Kortekaas, T., Koushik, A. N., Kraan, M., van de Kraats, M., Kranzhoff, S. L., Kuijer, P., Kukkadapu, K. A., Lam, K., Letendre, N., Li, P., Limburg, R., Linde, F., Locquet, J. -P., Loosen, P., Lueck, H., Martınez, M., Masserot, A., Meylahn, F., Molenaar, M., Mow-Lowry, C., Mundet, J., Munneke, B., van Nieuwland, L., Pacaud, E., Pascucci, D., Petit, S., Van Ranst, Z., Raskin, G., Recaman, P. M., van Remortel, N., Rolland, L., de Roo, L., Roose, E., Rosier, J. C., Ryckbosch, D., Schouteden, K., Sevrin, A., Sider, A., Singha, A., Spagnuolo, V., Stahl, A., Steinlechner, J., Steinlechner, S., Swinkels, B., Szilasi, N., Tacca, M., Thienpont, H., Vecchio, A., Verkooijen, H., Vermeer, C. H., Vervaeke, M., Visser, G., Walet, R., Werneke, P., Westhofen, C., Willke, B., Xhahi, A., Zhang, T.

论文摘要

与当前的晚期探测器相比,引力波观测值的第三代,例如爱因斯坦望远镜(ET)和宇宙资源管理器(CE),旨在提高敏感性至少10倍的敏感性。为了告知第三代探测器的设计并开发和合格其子系统,需要专门的测试设施。 EtPathfinder原型使用完整的干涉仪配置,并旨在在与ET的类似环境中提供高灵敏度设施。除了1550 nm和硅测试质量的干涉法外,Etpathfinder还将重点关注2090 nm的低温技术,激光器和光学元件和高级量子噪声还原方案。本文分析了基础噪声贡献,并将它们结合成两种最初靶向配置的完整噪声预算:1)以1550 nm激光光和18 k的温度和2)在2090 nm波长和温度为123 k的温度下运行。

The third-generation of gravitational wave observatories, such as the Einstein Telescope (ET) and Cosmic Explorer (CE), aim for an improvement in sensitivity of at least a factor of ten over a wide frequency range compared to the current advanced detectors. In order to inform the design of the third-generation detectors and to develop and qualify their subsystems, dedicated test facilities are required. ETpathfinder prototype uses full interferometer configurations and aims to provide a high sensitivity facility in a similar environment as ET. Along with the interferometry at 1550 nm and silicon test masses, ETpathfinder will focus on cryogenic technologies, lasers and optics at 2090 nm and advanced quantum-noise reduction schemes. This paper analyses the underpinning noise contributions and combines them into full noise budgets of the two initially targeted configurations: 1) operating with 1550 nm laser light and at a temperature of 18 K and 2) operating at 2090 nm wavelength and a temperature of 123 K.

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