Published June 7, 2008
| Published
Journal Article
Open
Demonstration of displacement-noise-free interferometry using bi-directional Mach–Zehnder interferometers
Chicago
Abstract
We have demonstrated displacement- and frequency-noise-free laser interferometry (DFI) by partially implementing a recently proposed optical configuration using bi-directional Mach–Zehnder interferometers (MZIs). This partial implementation, the minimum necessary to be called DFI, has confirmed the essential feature of DFI: the combination of two MZI signals can be carried out in a way that cancels the displacement noise of the mirrors and beam splitters while maintaining gravitational-wave signals. The attained maximum displacement noise suppression was 45 dB.
Additional Information
© Institute of Physics and IOP Publishing Limited 2008. Received 5 November 2007, in final form 25 January 2008. Published 15 May 2008. Print publication: Issue 11 (7 June 2008). This research was partially supported by the Japanese Ministry of Education, Culture, Sports, Science and Technology under Grant-in-Aid for Scientific Research (B), No 18340070, 2006. RLW was supported by the US National Science Foundation under Cooperative Agreement No PHY-0107417. The research of YC, AP and KS is supported by the Alexander von Humboldt Foundation's Sofja Kovalevskaja Programme (funded by the German Ministry of Education and Research). INVITED AMALDI TALK. Special issue: Proceedings of the 18th International Conference on General Relativity and Gravitation (GRG18) and 7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7), Sydney, Australia, July 2007 http://www.iop.org/EJ/toc/0264-9381/25/11Attached Files
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Additional details
- Eprint ID
- 10561
- Resolver ID
- CaltechAUTHORS:SATcqg08
- Ministry of Education, Culture, Sports, Science and Technology (MEXT)
- 18340070
- NSF
- PHY-0107417
- Alexander von Humboldt Foundation
- Created
-
2008-05-17Created from EPrint's datestamp field
- Updated
-
2022-07-12Created from EPrint's last_modified field
- Caltech groups
- LIGO