B Willke et al 2002 Class. Quantum Grav. 19 1377 doi:10.1088/0264-9381/19/7/321
B Willke1,3, P Aufmuth1, C Aulbert4, S Babak5, R Balasubramanian5, B W Barr2, S Berukoff4, S Bose4, G Cagnoli2, M M Casey2, D Churches5, D Clubley2, C N Colacino1, D R M Crooks2, C Cutler4, K Danzmann1,3, R Davies5, R Dupuis2, E Elliffe2, C Fallnich6, A Freise3, S Goßler1, A Grant2, H Grote3, G Heinzel1, A Heptonstall2, M Heurs1, M Hewitson2, J Hough2, O Jennrich2, K Kawabe3, K Kötter1, V Leonhardt1, H Lück1,3, M Malec1, P W McNamara2, S A McIntosh2, K Mossavi3, S Mohanty4, S Mukherjee4, S Nagano2, G P Newton2, B J Owen4, D Palmer2, M A Papa4, M V Plissi2, V Quetschke1, D I Robertson2, N A Robertson2, S Rowan2, A Rüdiger3, B S Sathyaprakash5, R Schilling3, B F Schutz4,5, R Senior5, A M Sintes4, K D Skeldon2, P Sneddon2, F Stief1, K A Strain2, I Taylor5, C I Torrie2, A Vecchio4,7, H Ward2, U Weiland1, H Welling6, P Williams4, W Winkler3, G Woan2 and I Zawischa6
Show affiliationsThe GEO 600 laser interferometer with 600 m armlength is part of a worldwide network of gravitational wave detectors. Due to the use of advanced technologies like multiple pendulum suspensions with a monolithic last stage and signal recycling, the anticipated sensitivity of GEO 600 is close to the initial sensitivity of detectors with several kilometres armlength. This paper describes the subsystems of GEO 600, the status of the detector by September 2001 and the plans towards the first science run.
Issue 7 (7 April 2002)
Received 2 October 2001, in final form 14 November 2001
Published 11 March 2002
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