ETpathfinder: a cryogenic testbed for interferometric gravitational-wave detectors

被引：5

作者：

Utina, A. ^{[1
,2
]}

Amato, A. ^{[1
,2
]}

Arends, J. ^{[3
]}

Arina, C. ^{[4
]}

de Baar, M. ^{[5
]}

Baars, M. ^{[2
]}

Baer, P. ^{[6
]}

van Bakel, N. ^{[2
]}

Beaumont, W. ^{[7
]}

Bertolini, A. ^{[2
]}

van Beuzekom, M. ^{[2
]}

Biersteker, S. ^{[3
]}

Binetti, A. ^{[8
]}

ter Brake, H. J. M. ^{[9
]}

Bruno, G. ^{[4
]}

Bryant, J. ^{[10
,11
]}

Bulten, H. J. ^{[2
]}

Busch, L. ^{[12
]}

Cebeci, P. ^{[6
]}

Collette, C. ^{[13
]}

Cooper, S. ^{[10
,11
]}

Cornelissen, R. ^{[2
]}

Cuijpers, P. ^{[1
]}

van Dael, M. ^{[5
]}

Danilishin, S. ^{[1
,2
]}

Diksha, D. ^{[1
,2
]}

van Doesburg, S. ^{[2
]}

Doets, M. ^{[2
]}

Elsinga, R. ^{[2
,3
]}

Erends, V ^{[2
]}

van Erps, J. ^{[14
,15
]}

Freise, A. ^{[2
,3
]}

Frenaij, H. ^{[2
]}

Garcia, R. ^{[16
,17
]}

Giesberts, M. ^{[6
]}

Grohmann, S. ^{[12
]}

Van Haevermaet, H. ^{[7
]}

Heijnen, S. ^{[2
]}

van Heijningen, J., V ^{[4
]}

Hennes, E. ^{[2
]}

Hennig, J-S ^{[1
,2
]}

Hennig, M. ^{[1
,2
]}

Hertog, T. ^{[8
]}

Hild, S. ^{[1
,2
]}

Hoffmann, H-D ^{[6
]}

Hoft, G. ^{[2
]}

Hopman, M. ^{[2
]}

Hoyland, D. ^{[10
,11
]}

Iandolo, G. A. ^{[1
,2
]}

Ietswaard, C. ^{[2
]}

机构：

[1] Maastricht Univ, Dept Gravitat Waves & Fundamental Phys, NL-6200 MD Maastricht, Netherlands

[2] Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands

[3] Vrije Univ Amsterdam, Dept Phys & Astron, VU Amsterdam, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands

[4] UCLouvain, Ctr Cosmol Particle Phys & Phenomenol CP3, B-1348 Louvain La Neuve, Belgium

[5] Eindhoven Univ Technol, NL-5612 AZ Eindhoven, Netherlands

[6] Fraunhofer ILT Inst Laser Technol, Steinbachstr 15, D-52074 Aachen, Germany

[7] Univ Antwerp, Prinsstr 13, B-2000 Antwerp, Belgium

[8] Katholieke Univ Leuven, Dept Phys & Astron, Celestijnenlaan 200D, B-3001 Leuven, Belgium

[9] Univ Twente, POB 217, NL-7500 AE Enschede, Netherlands

[10] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[11] Univ Birmingham, Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England

[12] Karlsruhe Inst Technol KIT, D-76131 Karlsruhe, Germany

[13] ULiege Precis Mechatron Lab, 9 Allee Decouverte, B-4000 Liege, Belgium

[14] Vrije Univ Brussel, Fac Engn, Dept Appl Phys & Photon TONA, Brussels Photon B PHOT, Pl Laan 2, B-1050 Brussels, Belgium

[15] FlandersMake, Pl Laan 2, B-1050 Brussels, Belgium

[16] Inst High Energy Phys Barcelona IFAE, Fac Ciencies Nord, Campus UAB, Barcelona 08193, Spain

[17] ICREA, Campus UAB, Barcelona 08193, Spain

[18] Univ Western Australia, OzGrav, Crawley, WA 6009, Australia

[19] Max Planck Inst Gravitat Phys AEI, Callinstr 38, D-30167 Hannover, Germany

[20] Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules LAPP, CNRS IN2P3, F-74941 Annecy, France

[21] Ghent Univ Gent, Dept Phys & Astron, Proeftuinstr 86, B-9000 Ghent, Belgium

[22] Vrije Univ Brussel, Theoret Nat Kunde, Pl Laan 2, B-1050 Brussels, Belgium

[23] Int Solvay Inst, Pl Laan 2, B-1050 Brussels, Belgium

[24] Rhein Westfal TH Aachen, Templergraben 55, D-52062 Aachen, Germany

来源：

CLASSICAL AND QUANTUM GRAVITY | 2022年 / 39卷 / 21期

关键词：

gravitational-wave detectors; third generation of gravitational-wave detectors; Einstein Telescope; Cosmic Explorer; Voyager; ETpathfinder; THERMAL NOISE; SILICON;

D O I：

10.1088/1361-6382/ac8fdb

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The third-generation (3G) of gravitational wave observatories, such as the Einstein Telescope (ET) and Cosmic Explorer, 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 3G 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.

引用

页数：23

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