Low weight mirror substrates

MacKay, Peter E.; Beveridge, N.; Wood, Trevor

doi:10.1117/12.2027864

Cited by 1 publication

(5 citation statements)

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“…The prototype mirror was polished to 37 nm root-mean-square (RMS) roughness and 149 nm peak-to-valley (PV) flatness and was cycled multiple times between -20 and 50°C. Excellent stability was seen with the RMS and PV values at 50°C being 35 nm and 152 nm [29]. This technique is also suitable for producing baseplates for ultra-stable optical sensing assemblies, as required for eLISA.…”

Section: Other Astronomical Applicationsmentioning

confidence: 80%

“…A considerable volume of work can be found in the literature on the strength of HCBs [9,13,16,18,19,21,22,25,26,29,[38][39][40][41]. In these studies, the strengths of bonds having a variety of different geometries are reported.…”

Section: Bond Strengthmentioning

confidence: 99%

“…Since then, work has been completed that suggests this is a viable approach, as discussed further in [29]. A composite lightweighted baseplate with hydroxide catalysis bonded interfaces is a design solution under consideration for eLISA.…”

Section: Elisamentioning

confidence: 99%

“…Mirror stability and mass are important design parameters with lightweighted low-expansion substrates of interest to form the mirrors. HCB has been used to create lightweight composite mirrors in a project between Gooch and Housego (UK) Ltd, Surrey Satellite Technology Ltd and the University of Glasgow [29]. Photographs of a prototype mirror are shown in Figure 9.…”

Section: Other Astronomical Applicationsmentioning

confidence: 99%

“…It was originally developed and patented for the Gravity Probe B space mission to assemble the fused silica star tracking telescope at Stanford University [7][8][9] and has since found its application in adapted form in gravitational wave (GW) detectors (both groundbased [10][11][12] and space-based [13,14]) as well as being considered for other applications in the field of astronomy [15][16][17][18][19][20][21][22][23][24] and beyond [25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Other Astronomical Applicationsmentioning

confidence: 80%