Challenges in thermal noise for 3rd generation of gravitational wave detectors

Nawrodt, R.; Rowan, S.; Punturo, M.; Ricci, F.; Vinet, J.-Y.

doi:10.1007/s10714-010-1066-5

Cited by 37 publications

(27 citation statements)

References 120 publications

(192 reference statements)

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“…Powerful and highly stable lasers around 1550 nm used in fiber-optic communication make this wavelength a good candidate for the use of silicon optics. Additionally, the low mechanical loss of silicon at cryogenic temperatures 1,2 suggests its use in low thermal noise experiments such as gravitational wave detectors 3,4 or cavities used for laser frequency stabilization. 5 Applications using optical components at high laser powers can suffer from thermal lensing effects.…”

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confidence: 99%

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Thermo-optic coefficient of silicon at 1550 nm and cryogenic temperatures

et al. 2012

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confidence: 99%

“…But at low temperatures the high mechanical loss 17 in fused silica precludes its use as a substrate material due to the increased Brownian thermal noise. 3 In contrast, silicon promises an effective noise reduction below 30 K as it shows a low mechanical loss and its thermo-optic coefficient drops below the room temperature value of fused silica.…”

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confidence: 99%

Thermo-optic coefficient of silicon at 1550 nm and cryogenic temperatures

et al. 2012

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“…Thermal noise basing on the change of the refractive index on temperature -thermorefractive (TR) noise -is one key noise process in the design of interferometric gravitational wave detectors [1][2][3]. Wherever the laser beam passes matter, the temperature fluctuations within the substrate will cause a change of the refractive index and, consequently, will change the phase of the traveling beam.…”

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confidence: 99%

Thermorefractive noise of finite-sized cylindrical test masses

et al. 2011

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We present an analytical solution for the effect of thermorefractive noise considering finite-sized cylindrical test masses. For crystalline materials at low temperatures the effect of finite dimensions becomes important. The calculations are independently performed using the FluctuationDissipation-Theorem and Langevin's approach. Our results are applied to the input test mass of the current and future cryogenic gravitational wave detectors CLIO, LCGT, and ET and are compared to the respective standard quantum limit. For a substrate temperature of 10 K we find that the thermorefractive noise amplitude of the silicon input test mass in ET is only a factor of 2 below the standard quantum limit for frequencies above 500 Hz. Thus, thermorefractive noise of the input test mass could become a severe limitation if one uses techniques to beat the standard quantum limit like, e.g., squeezing. In contrast the effect of thermorefractive noise of the input test mass is negligible for CLIO and LCGT.

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“…For possible future upgrades to these detectors and for new detectors, such as the detector in Japan, KAGRA [15,16] and the European detector concept, the Einstein Telescope (ET) [17][18][19], the cooling of the suspension down to cryogenic temperature may be employed as a method of reducing the level of thermal noise [20,21]. At low temperature, ∼ 40 K, fused silica exhibits high levels of dissipation, and therefore an alternative mirror and suspension material is required [22].…”

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confidence: 99%

Mechanical loss of a hydroxide catalysis bond between sapphire substrates and its effect on the sensitivity of future gravitational wave detectors

et al. 2016

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Mechanical loss of a hydroxide catalysis bond between sapphire substrates and its effect on the sensitivity of future gravitational wave detectors. Physical Review D, 94(8), 082003. (doi:10.1103/PhysRevD.94.082003) This is the author's final accepted version.There may be differences between this version and the published version. Hydroxide catalysis bonds are low mechanical loss joints which are used in the fused silica mirror suspensions of current room temperature interferometric gravitational wave detectors, one of the techniques which was essential to allow the recent detection of gravitational radiation by LIGO. More sensitive detectors may require cryogenic techniques with sapphire as a candidate mirror and suspension material and thus hydroxide catalysis bonds are under consideration for jointing sapphire. This paper presents the first measurements of the mechanical loss of such a bond created between sapphire substrates and measured down to cryogenic temperatures. The mechanical loss is found to be 0.03 ± 0.01 at room temperature, decreasing to (3 ± 1) × 10 −4 at 20 K. The resulting thermal noise of the bonds on several possible mirror suspensions is presented.

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Challenges in thermal noise for 3rd generation of gravitational wave detectors

Cited by 37 publications

References 120 publications

Thermo-optic coefficient of silicon at 1550 nm and cryogenic temperatures

Thermo-optic coefficient of silicon at 1550 nm and cryogenic temperatures

Thermorefractive noise of finite-sized cylindrical test masses

Mechanical loss of a hydroxide catalysis bond between sapphire substrates and its effect on the sensitivity of future gravitational wave detectors

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