Silica research in Glasgow

Barr, B.; Cagnoli, G.; Casey, M. M.; Clubley, D.; Crooks, D. R. M.; Danzmann, K.; Elliffe, E. J.; Goßler, S.; Grant, A.; Grote, H.; Heptonstall, A.; Jennrich, O.; Lück, H.; McIntosh, Steven; Newton, G.; Palmer, David A.; Plissi, M. V.; Robertson, D. I.; Robertson, N. A.; Rowan, S.; Skeldon, K. D.; Sneddon, P.; Strain, K. A.; Torrie, C. I.; Ward, H.; Willems, P. A.; Willke, B.; Winkler, W.

doi:10.1088/0264-9381/19/7/357

Cited by 17 publications

(15 citation statements)

References 10 publications

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“…In GEO600, a quasimonolithic suspension was pioneered using fused silica fibres attached to the side of the mirrors via interface pieces called 'ears' using HCB (see Figure 6) [10,33,66].…”

Section: Fused Silica Quasi-monolithic Mirror Suspensionsmentioning

confidence: 99%

Hydroxide catalysis bonding for astronomical instruments

Veggel

Killow

2014

Advanced Optical Technologies

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Hydroxide catalysis bonding (HCB) as a jointing technique has been under development for astronomical applications since ∼1998 (patented by D.-H. Gwo). It uses an aqueous hydroxide solution to form a chemical bond between oxide or oxidisable materials (e.g., SiO 2 , sapphire, silicon and SiC). It forms strong, extremely thin bonds, and is suitable for room temperature bonding, precision alignment, operation in ultra-low vacuum and down to temperatures of 2.5 K. It has been applied in the NASA satellite mission Gravity Probe B and in the ground-based gravitational wave (GW) detector GEO600. It will soon fly again on the ESA LISA Pathfinder mission and is currently being implemented in the Advanced LIGO and Virgo ground-based GW detectors. This technique is also of considerable interest for use in other astronomical fields and indeed more broadly, due to its desirable, and adjustable, combination of properties. This paper gives an overview of how HCB has been and can be applied in astronomical instruments, including an overview of the current literature on the properties of hydroxide catalysis bonds.

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“…In GEO600, a quasimonolithic suspension was pioneered using fused silica fibres attached to the side of the mirrors via interface pieces called 'ears' using HCB (see Figure 6) [10,33,66].…”

Section: Fused Silica Quasi-monolithic Mirror Suspensionsmentioning

confidence: 99%

Hydroxide catalysis bonding for astronomical instruments

Veggel

Killow

2014

Advanced Optical Technologies

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“…6a). Fused silica has been shown to have a low mechanical loss at room temperature with extensive studies having been carried to on the influence of the surface quality, and type of material on the mechanical loss [51,71,76,77,[92][93][94]. As mentioned earlier the measured mechanical loss of a sample can be considered to have components associated with both the surface and bulk of a samples with the intrinsic bulk loss potentially being as low as 4 × 10 −10 at 100 Hz [51].…”

Section: Fused Silicamentioning

confidence: 99%

“…A monolithic suspension is preferred due to the ability of avoiding excess losses from the contact points of different materials. This approach has been successfully implemented in the suspensions of the GEO600 detector [75,76], and is planned for use in 2nd generation gravitational wave detectors (see, e.g. [40,72,74,77,78]).…”

Section: Current Status Of the Suspension Thermal Noisementioning

confidence: 99%

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

et al. 2010

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Various noise sources limit the sensitivity of current interferometric gravitational wave detectors, including seismic noise, thermal noise of the optical components and suspension elements and photon shot noise. Plans are in place for a suite of hardware upgrades which should increase the sensitivity of these detectors by reducing the various noise sources. With these designs for 2nd generation detectors mature, techniques for further improvement of detector sensitivity by a factor of approximately 10 are under study. A particular challenge is the reduction of the thermal noise associated with the interferometer mirrors and their suspensions. We review the current status of research on thermal noise in interferometric gravitational wave detectors. Aspects of possible techniques for use in future '3rd generation detectors' such as cryogenics and diffractive optics are discussed

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“…The monolithic suspension consists of the mirror and the intermediate mass, both made of fused silica and four fused silica fibres of diameter 300 µm [2]. With the technique of silicate bonding two 'ears' are attached to each mass [6].…”

Section: The Main Suspensionmentioning

confidence: 99%

The modecleaner system and suspension aspects of GEO 600

Goßler

Casey

Freise

et al. 2002

Class. Quantum Grav.

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GEO 600 uses two 8 m triangular ring cavities as a modecleaner system for the stabilization of the laser. To isolate the cavities with respect to the seismic noise the optical components are suspended as double pendulums. The resonances of these pendulums are damped by a local-control loop via magnet-coil actuators acting on the intermediate masses. The suspension scheme and the measured key data (i.e. finesse, linewidth, visibility, throughput and in-lock durations of the cavities, as well as the isolation performance and the resulting frequency stability) of the modecleaner system will be given in this paper. Furthermore an overview of the GEO 600 interferometer suspension will be given. PACS numbers: 0480N, 9555Y

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Silica research in Glasgow

Cited by 17 publications

References 10 publications

Hydroxide catalysis bonding for astronomical instruments

Hydroxide catalysis bonding for astronomical instruments

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

The modecleaner system and suspension aspects of GEO 600

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