A Freise et al 2002 Class. Quantum Grav. 19 1389 doi:10.1088/0264-9381/19/7/322
A Freise1, M M Casey3, S Gossler1, H Grote1, G Heinzel2, H Lück1,2, D I Robertson3, K A Strain3, H Ward3, B Willke1,2, J Hough3 and K Danzmann1,2
Show affiliationsUsing one arm of the Michelson interferometer and the power recycling mirror of the interferometric gravitational wave detector GEO 600, we created a Fabry–Perot cavity with a length of 1200 m. The main purpose of this experiment was to gather first experience with the main optics, its suspensions and the corresponding control systems. The residual displacement of a main mirror is about 150 nm rms. By stabilizing the length of the 1200 m long cavity to the pre-stabilized laser beam, we achieved an error point frequency noise of 100 μHz Hz−1/2 at 100 Hz Fourier frequency. In addition we demonstrated the reliable performance of all included subsystems by several 10-hour-periods of continuous stable operation. Thus the full frequency stabilization scheme for GEO 600 was successfully tested.
78A60 Lasers, masers, optical bistability, nonlinear optics (See also 81V80)
Instrumentation and measurement
Issue 7 (7 April 2002)
Received 3 October 2001, in final form 8 November 2001
Published 11 March 2002
A Freise et al 2002 Class. Quantum Grav. 19 1389
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