دورية أكاديمية
E-TEST: a compact low-frequency isolator for a large cryogenic mirror
| العنوان: | E-TEST: a compact low-frequency isolator for a large cryogenic mirror |
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| المؤلفون: | Sider, Ameer, Di Fronzo, Chiara, Amez-Droz, Loïc, Amorosi, Anthony, Badaracco, Francesca, Baer, Patrick, Bertolini, Alessandro, Bruno, Giacomo, Cebeci, Pelin, Collette, Christophe, Ebert, Johannes, Erben, Benjamin, Esteves, Rui, Ferreira, Elvis, Gatti, Alberto, Giesberts, Martin, Hebbeker, Thomas, van Heijningen, Joris, Hennig, Jan-Simon, Hennig, Margot, Hild, Stefan, Hoefer, Marco, Hoffmann, Hans-Dieter, Jamshidi, Rasa, Jacques, Lionel, Joppe, Robert, Kuhlbusch, Tim, Lakkis, Mouhamad Haidar, Lenaerts, Cedric, Locquet, Jean-Pierre, Loicq, Jerôme, Le Van, Bao, Loosen, Peter, Nesladek, Milos, Reiter, Melina, Stahl, Achim, Steinlechner, Jessia, Steinlechner, Sebastian, Tavernier, Filip, Teloi, Mayana, Vilaboa Perez, Jesus, Zeoli, Morgane |
| المصدر: | Classical and Quantum Gravity (2023-06-27) |
| بيانات النشر: | IOP Publishing, 2023. |
| سنة النشر: | 2023 |
| مصطلحات موضوعية: | E-TEST, radiative cooling, silicon mirror, coating, cryogenic sensor, active control, seismic, Engineering, computing & technology, Aerospace & aeronautics engineering, Ingénierie, informatique & technologie, Ingénierie aérospatiale |
| الوصف: | Abstract To achieve the expected level of sensitivity of third-generationgravitational-wave observatories, more accurate and sensitive instruments than those of the second generation must be used to reduce all sources of noise.Amongst them, one of the most relevant is seismic noise, which will require thedevelopment of a better isolation system, especially at low frequencies (below 10Hz), the operation of large cryogenic silicon mirrors, and the improvement ofoptical wavelength readouts. In this framework, this article presents the activitiesof the E-TEST (Einstein Telescope Euregio Meuse-Rhine Site & Technology) todevelop and test new key technologies for the next generation of GW observatories.A compact isolator system for a large silicon mirror at a low frequency is proposed. The design of the isolator allows the overall heightof the isolation system to be significantly compact and also suppresses seismicnoise at low frequencies. To minimize the effect of thermal noise, the isolationsystem is provided with a 100-kg silicon mirror which is suspended in a vacuumchamber at cryogenic temperature (25-40 K). To achieve this temperature withoutinducing vibrations to the mirror, a radiation-based cooling strategy is employed.In addition, cryogenic sensors and electronics are being developed as part of theE-TEST to detect vibrational motion in the penultimate cryogenic stage. Sincethe used silicon material is not transparent below the wavelengthstypically used for GW detectors, new optical components andlasers must be developed in the range above 1500 nm to reduce absorption andscattering losses. Therefore, solid-state and fiber lasers with a wavelength of 2090nm, matching high-efficiency photodiodes, and low-noise crystalline coatings arebeing developed. Accordingly, the key technologies provided by E-TEST servecrucially to reduce the limitations of the current generation of GW observatoriesand to determine the technical design for the next generation. |
| نوع الوثيقة: | journal article http://purl.org/coar/resource_type/c_6501Test article peer reviewed |
| اللغة: | English |
| العلاقة: | https://iopscience.iop.org/article/10.1088/1361-6382/ace230Test; urn:issn:0264-9381; urn:issn:1361-6382 |
| DOI: | 10.1088/1361-6382/ace230 |
| الوصول الحر: | https://orbi.uliege.be/handle/2268/305597Test |
| حقوق: | open access http://purl.org/coar/access_right/c_abf2Test info:eu-repo/semantics/openAccess |
| رقم الانضمام: | edsorb.305597 |
| قاعدة البيانات: | ORBi |
| DOI: | 10.1088/1361-6382/ace230 |
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