E-TEST: a compact low-frequency isolator for a large cryogenic mirror

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

doi:10.1088/1361-6382/ace230

E-TEST: a compact low-frequency isolator for a large cryogenic mirror

A. Sider
, C. Di Fronzo
, L. Amez-Droz
, A. Amorosi
, F. Badaracco
, P. Baer
, A. Bertolini
, G. Bruno
, P. Cebeci
, C. Collette
, J. Ebert
, B. Erben
, R. Esteves
, E. Ferreira
, A. Gatti
, M. Giesberts
, T. Hebbeker
, J.V. van Heijningen
, J.-S. Hennig
, M. Hennig

S. Hild, M. Hoefer, H.-D. Hoffmann, L. Jacques, R. Jamshidi, R. Joppe, T.-J. Kuhlbusch, M.H. Lakkis, C. Lenaerts, J.-P. Locquet, J. Loicq, B Long Le Van, P. Loosen, M. Nesladek, M. Reiter, A. Stahl, J. Steinlechner, S. Steinlechner, F. Tavernier, M. Teloi, J. Vilaboa Pérez, M. Zeoli

Research output: Contribution to Journal › Article › Academic › peer-review

Abstract

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 determine the technical design for the next generation.

Original language	English
Article number	165002
Journal	Classical and Quantum Gravity
Volume	40
Issue number	16
DOIs	https://doi.org/10.1088/1361-6382/ace230
Publication status	Published - 31 Aug 2023
Externally published	Yes

Funding

This work comes within the scope of the E-TEST project, which is carried out within the framework of the Interreg V-A Euregio Meuse-Rhine Programme, with million from the European Regional Development Fund (ERDF). By investing EU funds in Interreg projects, the European Union is investing directly in economic development, innovation, territorial development, social inclusion, and education in the Euregio Meuse-Rhine region. For a thorough review, the authors would like to thank European Union for this support and investment. This paper can be referenced to this LIGO DCC Number LIGO-P2200399. This work comes within the scope of the E-TEST project, which is carried out within the framework of the Interreg V-A Euregio Meuse-Rhine Programme, with 7 , 5 million from the European Regional Development Fund (ERDF). By investing EU funds in Interreg projects, the European Union is investing directly in economic development, innovation, territorial development, social inclusion, and education in the Euregio Meuse-Rhine region. For a thorough review, the authors would like to thank European Union for this support and investment. This paper can be referenced to this LIGO DCC Number LIGO-P2200399.

Funders	Funder number
European Commission	LIGO-P2200399
European Regional Development Fund

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10.1088/1361-6382/ace230

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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., ... Zeoli, M. (2023). E-TEST: a compact low-frequency isolator for a large cryogenic mirror. Classical and Quantum Gravity, 40(16), Article 165002. https://doi.org/10.1088/1361-6382/ace230

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title = "E-TEST: a compact low-frequency isolator for a large cryogenic mirror",

abstract = "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 determine the technical design for the next generation.",

author = "A. Sider and \{Di Fronzo\}, C. and L. Amez-Droz and A. Amorosi and F. Badaracco and P. Baer and A. Bertolini and G. Bruno and P. Cebeci and C. Collette and J. Ebert and B. Erben and R. Esteves and E. Ferreira and A. Gatti and M. Giesberts and T. Hebbeker and \{van Heijningen\}, J.V. and J.-S. Hennig and M. Hennig and S. Hild and M. Hoefer and H.-D. Hoffmann and L. Jacques and R. Jamshidi and R. Joppe and T.-J. Kuhlbusch and M.H. Lakkis and C. Lenaerts and J.-P. Locquet and J. Loicq and \{Le Van\}, \{B Long\} and P. Loosen and M. Nesladek and M. Reiter and A. Stahl and J. Steinlechner and S. Steinlechner and F. Tavernier and M. Teloi and \{Vilaboa P{\'e}rez\}, J. and M. Zeoli",

year = "2023",

month = aug,

day = "31",

doi = "10.1088/1361-6382/ace230",

language = "English",

volume = "40",

journal = "Classical and Quantum Gravity",

issn = "0264-9381",

publisher = "IOP Publishing Ltd.",

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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, JV, Hennig, J-S, Hennig, M, Hild, S, Hoefer, M, Hoffmann, H-D, Jacques, L, Jamshidi, R, Joppe, R, Kuhlbusch, T-J, Lakkis, MH, Lenaerts, C, Locquet, J-P, Loicq, J, Le Van, BL, Loosen, P, Nesladek, M, Reiter, M, Stahl, A, Steinlechner, J, Steinlechner, S, Tavernier, F, Teloi, M, Vilaboa Pérez, J & Zeoli, M 2023, 'E-TEST: a compact low-frequency isolator for a large cryogenic mirror', Classical and Quantum Gravity, vol. 40, no. 16, 165002. https://doi.org/10.1088/1361-6382/ace230

TY - JOUR

T1 - E-TEST

T2 - a compact low-frequency isolator for a large cryogenic mirror

AU - Sider, A.

AU - Di Fronzo, C.

AU - Amez-Droz, L.

AU - Amorosi, A.

AU - Badaracco, F.

AU - Baer, P.

AU - Bertolini, A.

AU - Bruno, G.

AU - Cebeci, P.

AU - Collette, C.

AU - Ebert, J.

AU - Erben, B.

AU - Esteves, R.

AU - Ferreira, E.

AU - Gatti, A.

AU - Giesberts, M.

AU - Hebbeker, T.

AU - van Heijningen, J.V.

AU - Hennig, J.-S.

AU - Hennig, M.

AU - Hild, S.

AU - Hoefer, M.

AU - Hoffmann, H.-D.

AU - Jacques, L.

AU - Jamshidi, R.

AU - Joppe, R.

AU - Kuhlbusch, T.-J.

AU - Lakkis, M.H.

AU - Lenaerts, C.

AU - Locquet, J.-P.

AU - Loicq, J.

AU - Le Van, B Long

AU - Loosen, P.

AU - Nesladek, M.

AU - Reiter, M.

AU - Stahl, A.

AU - Steinlechner, J.

AU - Steinlechner, S.

AU - Tavernier, F.

AU - Teloi, M.

AU - Vilaboa Pérez, J.

AU - Zeoli, M.

PY - 2023/8/31

Y1 - 2023/8/31

N2 - 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 determine the technical design for the next generation.

AB - 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 determine the technical design for the next generation.

UR - https://www.scopus.com/pages/publications/85165380295

U2 - 10.1088/1361-6382/ace230

DO - 10.1088/1361-6382/ace230

M3 - Article

SN - 0264-9381

VL - 40

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

IS - 16

M1 - 165002

ER -

E-TEST: a compact low-frequency isolator for a large cryogenic mirror

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