Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors

TL;DR

This paper introduces an adjustable, picometer-stable interferometer design that simplifies assembly and testing for space-based gravitational wave detectors, maintaining high stability with flexible optical component placement.

Contribution

The authors present a novel opto-mechanical concept with adjustable mounts that achieves picometer stability, enabling faster assembly and testing of interferometers for space applications.

Findings

Achieved cavity length noise below 1 pm/√Hz down to 3 mHz.

Verified the stability of the adjustable interferometer design.

Demonstrated suitability for space-based gravitational wave detection.

Abstract

Space-based gravitational wave detectors, such as the Laser Interferometer Space Antenna (LISA), use picometer-precision laser interferometry to detect gravitational waves at frequencies from 1 Hz down to below 0.1 mHz. Laser interferometers used for on-ground prototyping and testing of such instruments are typically constructed by permanently bonding or gluing optics onto an ultra-stable bench made of low-expansion glass ceramic. This design minimizes temperature coupling to length and tilt, which dominates the noise at low frequencies due to finite temperature stability achievable in laboratories and vacuum environments. Here, we present the study of an alternative opto-mechanical concept where optical components are placed with adjustable and freely positionable mounts on an ultra-stable bench, while maintaining picometer length stability. With this concept, a given interferometer configuration can be realised very quickly due to a simplified and speed-up assembly process, reducing the realisation time from weeks or months to a matter of hours. We built a corresponding test facility and verified the length stability of our concept by measuring the length change in an optical cavity that was probed with two different locking schemes, heterodyne laser frequency stabilisation and Pound-Drever-Hall locking. We studied the limitations of both locking schemes and verified that the cavity length noise is below 1 pm/sqrt(Hz) for frequencies down to 3 mHz. We thereby demonstrate that our concept can simplify the testing of interferometer configurations and opto-mechanical components and is suitable to realise flexible optical ground support equipment for space missions that use laser interferometry, such as future space-based gravitational wave detectors and satellite geodesy missions.