Optical detector topology for third-generation gravitational wave observatories

被引：6

作者：

Freise, Andreas ^{[1
]}

Hild, Stefan ^{[2
]}

Somiya, Kentaro ^{[3
]}

Strain, Ken A. ^{[2
]}

Vicere, Andrea ^{[4
]}

Barsuglia, Matteo ^{[5
]}

Chelkowski, Simon ^{[1
]}

机构：

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

[2] Univ Glasgow, Inst Gravitat Res, Glasgow G12 8QQ, Lanark, Scotland

[3] CALTECH, Pasadena, CA 91125 USA

[4] Univ Urbino Carlo Bo, INFN, Sez Firenze, Urbino, Italy

[5] CNRS, UMR7164, Paris, France

来源：

GENERAL RELATIVITY AND GRAVITATION | 2011年 / 43卷 / 02期

基金：

日本学术振兴会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

Gravitational wave detector; Laser interferometer; Topology; Optical design; THERMAL NOISE; SUSPENSION; INTERFEROMETER; GENERATION; MODE;

D O I：

10.1007/s10714-010-1018-0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The third generation of gravitational wave observatories, with the aim of providing 100 times better sensitivity than currently operating interferometers, is expected to establish the evolving field of gravitational wave astronomy. A key element, required to achieve this ambitious sensitivity goal, is the exploration of new interferometer geometries, topologies and configurations. In this article we review the current status of the ongoing design work for third-generation gravitational wave observatories. The main focus is the evaluation of the detector geometry and detector topology. In addition we discuss some promising detector configurations and potential noise reduction schemes.

引用

页码：537 / 567

页数：31

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