المؤلفون: Sider, Ameer, Amez-Droz, Loïc, Amorosi, Anthony, Badaracco, F., Baer, P., Bruno, G., Bertolini, A., Collette, Christophe, Cebeci, P., Di Fronzo, Chiara, Ebert, J., Erben, B., Esteves, R., Ferreira, E., Gatti, A., Giesberts, M., Hebbeker, T., Hennig, J. S., Hennig, M., Hild, S., Hoefer, M., Hoffmann, H. D., Jacques, Lionel, Jamshidi, Rasa, {"lastName":"Joppe","firstNames":"R."}, Kuhlbusch, T., Lenaert, C., Lakkis, Mouhamad Haidar, Le Van, B. L., Loicq, J., Locquet, J. P., Loosen, P., Nesladek, M., Reiter, M., Stahl, A., Steinlechner, J., Steinlechner, S., Teloi, Mayana, {"lastName":"Vilaboa Perez", "firstNames"}, van Heijningen, J., Zeoli, Morgane

مصطلحات موضوعية: astro-ph.IM, General Relativity and Quantum Cosmology, E-TEST, active control, seismic, cryogenic sensor, radiative cooling, silicon mirror, coating, Engineering, computing & technology, Aerospace & aeronautics engineering, Ingénierie, informatique & technologie, Ingénierie aérospatiale

الوصف: E-TEST (Einstein Telescope Euregio-Meuse-Rhin Site and Technology) is aproject recently funded by the European program Ineterreg Euregio Meuse-Rhine.This program is dedicated to innovative cross boarder activities betweenBelgium, The Netherlands and Germany. With a total budget of15MC and aconsortium of 11 partners from the three countries, the objective of theproject is twofold. Firstly, to develop an eco-friendly and non-invasiveimaging of the geological conditions as well as the development of anobservatory of the underground in the EMR region. Secondly, to developtechnologies necessary for 3rd generation gravitational wave detectors. Inparticular, it is proposed to develop a prototype of large suspended cryogenicsilicon mirror, isolated from seismic vibrations at low frequency. The totalbudget of the project is equally spread over the two activities. The firstactivity is not discussed at all in this report. The E-TEST prototype will havesome key unique features: a silicon mirror of 100 kg, a radiative coolingstrategy (non contact), a low-frequency hybrid isolation stage, cryogenicsensors and electronics, a laser and optics at 2 microns, a low thermal noisecoating.

الوصول الحر: https://orbi.uliege.be/handle/2268/303703Test

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)

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.

العلاقة: https://iopscience.iop.org/article/10.1088/1361-6382/ace230Test; urn:issn:0264-9381; urn:issn:1361-6382

الوصول الحر: https://orbi.uliege.be/handle/2268/305597Test

المؤلفون: Sider, A., Di Fronzo, C., Amez-Droz, L., Amorosi, A., Badaracco, F., Baer, P., Bertolini, A., Bruno, G., Cebeci, P., Collette, C., Ebert, J., Erben, B., Esteves, R., Ferreira, E., Gatti, A., Giesberts, M., Hebbeker, T., van Heijningen, J., V, Hennig, J-S, Hennig, M., Hild, S., Hoefer, M., Hoffmann, H-D, Jacques, L., Jamshidi, R., Joppe, R., Kuhlbusch, T-J, Lakkis, M. H., Lenaerts, C., Locquet, J-P, Loicq, J., Le Van, B. Long, Loosen, P., NESLADEK, Milos, Reiter, M., Stahl, A., Steinlechner, J., Steinlechner, S., Tavernier, F., Teloi, M., Perez, J. Vilaboa, Zeoli, M.

المساهمون: Sider, A., Di Fronzo, C., Amez-Droz, L., Amorosi, A., Badaracco, F., Baer, P., Bertolini, A., Bruno, G., Cebeci, P., Collette, C., Ebert, J., Erben, B., Esteves, R., Ferreira, E., Gatti, A., Giesberts, M., Hebbeker, T., van Heijningen, J., V, Hennig, J-S, Hennig, M., Hild, S., Hoefer, M., Hoffmann, H-D, Jacques, L., Jamshidi, R., Joppe, R., Kuhlbusch, T-J, Lakkis, M. H., Lenaerts, C., Locquet, J-P, Loicq, J., Le Van, B. Long, Loosen, P., NESLADEK, Milos, Reiter, M., Stahl, A., Steinlechner, J., Steinlechner, S., Tavernier, F., Teloi, M., Perez, J. Vilaboa, Zeoli, M.

مصطلحات موضوعية: E-TEST, active control, seismic, cryogenic sensor, radiative cooling, silicon mirror, coating

الوصف: To achieve the expected level of sensitivity of third-generation gravitational-ave (GW) observatories, more accurate and sensitive instruments than those of the second generation must be used to reduce all sources of noises. Amongst them, one of the most relevant is seismic noise, which will require the development of a better isolation system, especially at low frequencies (below 10 Hz), the operation of large cryogenic silicon mirrors, and the improvement of optical wavelength readouts. In this framework, this article presents the activities of the E-TEST (Einstein Telescope Euregio Meuse-Rhine Site & Technology) to develop and test new key technologies for the next generation of GW observatories. A compact isolator system for a large silicon mirror (100 kg) at low frequency (<10 Hz) is proposed. The design of the isolator allows the overall height of the isolation system to be significantly compact and also suppresses seismic noise at low frequencies. To minimize the effect of thermal noise, the isolation system is provided with a 100 kg silicon mirror which is suspended in a vacuum chamber at cryogenic temperature (25-40 K). To achieve this temperature without inducing vibrations to the mirror, a radiation-based cooling strategy is employed. In addition, cryogenic sensors and electronics are being developed as part of the E-TEST to detect vibrational motion in the penultimate cryogenic stage. Since the commonly used silicon material is not transparent below the wavelengths typically used in the 1 mu m range for GW detectors, new optical components and lasers must be developed in the range above 1500 nm to reduce absorption and scattering losses. Therefore, solid-state and fiber lasers with a wavelength of 2090 nm, matching high-efficiency photodiodes, and low-noise crystalline coatings are being developed. Accordingly, the key technologies provided by E-TEST serve crucially to reduce the limitations of the current generation of GW observatories and to determine the technical design for the next ...

وصف الملف: application/pdf

العلاقة: CLASSICAL AND QUANTUM GRAVITY, 40 (16) (Art N° 165002); http://hdl.handle.net/1942/40754Test; 16; 40; 001027305600001

الإتاحة: https://doi.org/10.1088/1361-6382/ace230Test
http://hdl.handle.net/1942/40754Test

المؤلفون: Zhe Wang, Lingqi Wu, Yuanyuan Fang, Aihuan Dun, Jiaoling Zhao, Xueke Xu, Xiaolei Zhu

المصدر: Micromachines; Volume 13; Issue 2; Pages: 318

مصطلحات موضوعية: ion beam figuring, monocrystalline silicon mirror, flow field analysis, ultra-smooth surface

الوصف: X-ray free-electron lasers are large modern scientific devices that play an important role in fields such as frontier physics and biomedicine. In this study, a light source is connected to an experimental station through beam lines, which requires numerous ultra-smooth and high-precision X-ray mirrors. Monocrystalline silicon is an ideal substrate material where ion-beam figuring is required. However, the ultra-smooth surface is damaged after the ion-beam figuring. Through an analysis of the machined surface, it is found that in the process of vacuum pumping, the impurities in the cavity adhere to the machined surface and increase the roughness after processing. Therefore, an optimized vacuum-pumping scheme is proposed. The experiment demonstrates that the original value of the processed surface roughness remains unchanged.

وصف الملف: application/pdf

العلاقة: E：Engineering and Technology; https://dx.doi.org/10.3390/mi13020318Test

الإتاحة: https://doi.org/10.3390/mi13020318Test

المؤلفون: Atsushi Murakami, Hitosi Ohmori, Shaohui Yin, Touru Suzuki, Weimin Lin, Yoshihiro Uehara, 上原 嘉宏, 大森 整, 尹 韶輝, 村上 淳, 林 偉民, 鈴木 亨

المصدر: Proceedings of JSPE Semestrial Meeting. 2005, :777

المؤلفون: Junichi Uchikoshi, Mizuho Morita, Taichiro Okamoto, shoichi Shimada, 岡本 太一朗, 島田 尚一, 打越 純一, 森田 瑞穂

المصدر: Proceedings of JSPE Semestrial Meeting. 2003, :530

المؤلفون: Junichi Utikosi, Shoichi Simada, Taichiro Okamoto, 岡本 太一朗, 島田 尚一, 打越 純一

المصدر: Proceedings of JSPE Semestrial Meeting. 2002, :658

المؤلفون: H. Ohmori, S. Yin, W. Lin, Y. Uehara

المصدر: Proceedings of International Conference on Leading Edge Manufacturing in 21st century : LEM21. 2005, :733

مستخلص: To achieve the expected level of sensitivity of third-generation gravitational-wave (GW) observatories, more accurate and sensitive instruments than those of the second generation must be used to reduce all sources of noises. Amongst them, one of the most relevant is seismic noise, which will require the development of a better isolation system, especially at low frequencies (below 10 Hz), the operation of large cryogenic silicon mirrors, and the improvement of optical wavelength readouts. In this framework, this article presents the activities of the E-TEST (Einstein Telescope Euregio Meuse-Rhine Site & Technology) to develop and test new key technologies for the next generation of GW observatories. A compact isolator system for a large silicon mirror (100 kg) at low frequency ( < 10 Hz) is proposed. The design of the isolator allows the overall height of the isolation system to be significantly compact and also suppresses seismic noise at low frequencies. To minimize the effect of thermal noise, the isolation system is provided with a 100 kg silicon mirror which is suspended in a vacuum chamber at cryogenic temperature (25-40 K). To achieve this temperature without inducing vibrations to the mirror, a radiation-based cooling strategy is employed. In addition, cryogenic sensors and electronics are being developed as part of the E-TEST to detect vibrational motion in the penultimate cryogenic stage. Since the commonly used silicon material is not transparent below the wavelengths typically used in the 1 µm range for GW detectors, new optical components and lasers must be developed in the range above 1500 nm to reduce absorption and scattering losses. Therefore, solid-state and fiber lasers with a wavelength of 2090 nm, matching high-efficiency photodiodes, and low-noise crystalline coatings are being developed. Accordingly, the key technologies provided by E-TEST serve crucially to reduce the limitations of the current generation of GW observatories and to
Spaceborne Instrumentation

مصطلحات الفهرس: active control, coating, cryogenic sensor, E-TEST, radiative cooling, seismic, silicon mirror, journal article

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Classical and Quantum Gravity--0264-9381--88ee6259-ea35-4dcc-8b69-5dc656550e6f