Thermally induced refractive index fluctuations in transmissive optical components and their influence on the sensitivity of Einstein telescope

Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung › Peer-Review

Autorschaft

  • Jan Meyer
  • Walter Dickmann
  • Stefanie Kroker
  • Mika Gaedtke
  • Johannes Dickmann

Externe Organisationen

  • Technische Universität Braunschweig
  • Laboratory for Emerging Nanometrology Braunschweig (LENA)
  • Physikalisch-Technische Bundesanstalt (PTB)
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Details

OriginalspracheEnglisch
Aufsatznummer135001
FachzeitschriftClassical and quantum gravity
Jahrgang39
Ausgabenummer13
Frühes Online-Datum31 Mai 2022
PublikationsstatusVeröffentlicht - 7 Juli 2022
Extern publiziertJa

Abstract

With a relative length measurement precision of better than 10-23, gravitational wave interferometers are the most precise instruments that have ever been built. With this enormous sensitivity many noise sources potentially effect gravitational wave detector sensitivity, each of which must be investigated to ensure confidence in design sensitivity. We present calculations of photoelastic noise as well as thermo refractive noise in the beam splitter and the input test masses in Einstein telescope (ET). It turns out that the amplitude of the photoelastic noise in the ET low-frequency detector is about five orders of magnitude below the maximum design sensitivity and five orders of magnitude below that of the ET high-frequency detector, whereas thermo refractive noise impairs the design sensitivity by approximately 20%.

ASJC Scopus Sachgebiete

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Thermally induced refractive index fluctuations in transmissive optical components and their influence on the sensitivity of Einstein telescope. / Meyer, Jan; Dickmann, Walter; Kroker, Stefanie et al.
in: Classical and quantum gravity, Jahrgang 39, Nr. 13, 135001, 07.07.2022.

Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung › Peer-Review

Meyer J, Dickmann W, Kroker S, Gaedtke M, Dickmann J. Thermally induced refractive index fluctuations in transmissive optical components and their influence on the sensitivity of Einstein telescope. Classical and quantum gravity. 2022 Jul 7;39(13):135001. Epub 2022 Mai 31. doi: 10.1088/1361-6382/ac6e21
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abstract = "With a relative length measurement precision of better than 10-23, gravitational wave interferometers are the most precise instruments that have ever been built. With this enormous sensitivity many noise sources potentially effect gravitational wave detector sensitivity, each of which must be investigated to ensure confidence in design sensitivity. We present calculations of photoelastic noise as well as thermo refractive noise in the beam splitter and the input test masses in Einstein telescope (ET). It turns out that the amplitude of the photoelastic noise in the ET low-frequency detector is about five orders of magnitude below the maximum design sensitivity and five orders of magnitude below that of the ET high-frequency detector, whereas thermo refractive noise impairs the design sensitivity by approximately 20%.",
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AU - Meyer, Jan

AU - Dickmann, Walter

AU - Kroker, Stefanie

AU - Gaedtke, Mika

AU - Dickmann, Johannes

N1 - Funding Information: This work is partially funded by the Project 17FUN05 ‘PhotOQuant’ within the Programme EMPIR. The EMPIR initiative is co-founded by the European Union’s Horizon 2020 Research and Innovation Program and the EMPIR Participating Countries. The authors also acknowledge support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germanys Excellence Strategy—EXC-2123 QuantumFrontiers—390837967.

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AB - With a relative length measurement precision of better than 10-23, gravitational wave interferometers are the most precise instruments that have ever been built. With this enormous sensitivity many noise sources potentially effect gravitational wave detector sensitivity, each of which must be investigated to ensure confidence in design sensitivity. We present calculations of photoelastic noise as well as thermo refractive noise in the beam splitter and the input test masses in Einstein telescope (ET). It turns out that the amplitude of the photoelastic noise in the ET low-frequency detector is about five orders of magnitude below the maximum design sensitivity and five orders of magnitude below that of the ET high-frequency detector, whereas thermo refractive noise impairs the design sensitivity by approximately 20%.

KW - photoelasticity

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