Coupling of relative intensity noise and pathlength noise to the length measurement in the optical metrology system of LISA Pathfinder

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dc.identifier.uri http://dx.doi.org/10.15488/1702
dc.identifier.uri http://www.repo.uni-hannover.de/handle/123456789/1727
dc.contributor.author Wittchen, A.
dc.contributor.author et al.
dc.contributor.author LPF Collaboration
dc.date.accessioned 2017-07-17T07:53:16Z
dc.date.available 2017-07-17T07:53:16Z
dc.date.issued 2017
dc.identifier.citation Wittchen, A.; et al. (The LPF Collaboration): Coupling of relative intensity noise and pathlength noise to the length measurement in the optical metrology system of LISA Pathfinder. In: Journal of Physics: Conference Series 840 (2017), Nr. 1, 12003. DOI: https://doi.org/10.1088/1742-6596/840/1/012003
dc.description.abstract LISA Pathfinder is a technology demonstration mission for the space-based gravitational wave observatory, LISA. It demonstrated that the performance requirements for the interferometric measurement of two test masses in free fall can be met. An important part of the data analysis is to identify the limiting noise sources. [1] This measurement is performed with heterodyne interferometry. The performance of this optical metrology system (OMS) at high frequencies is limited by sensing noise. One such noise source is Relative Intensity Noise (RIN). RIN is a property of the laser, and the photodiode current generated by the interferometer signal contains frequency dependant RIN. From this electric signal the phasemeter calculates the phase change and laser power, and the coupling of RIN into the measurement signal depends on the noise frequency. RIN at DC, at the heterodyne frequency and at two times the heterodyne frequency couples into the phase. Another important noise at high frequencies is path length noise. To reduce the impact this noise is suppressed with a control loop. Path length noise not suppressed will couple directly into the length measurement. The subtraction techniques of both noise sources depend on the phase difference between the reference signal and the measurement signal, and thus on the test mass position. During normal operations we position the test mass at the interferometric zero, which is optimal for noise subtraction purposes. This paper will show results from an in-flight experiment where the test mass position was changed to make the position dependant noise visible. eng
dc.description.sponsorship Federal Ministry for Economic Affairs and Energy/FKZ/50OQ0501
dc.description.sponsorship Federal Ministry for Economic Affairs and Energy/FKZ/50OQ1601
dc.language.iso eng
dc.publisher Bristol : Institute of Physics Publishing
dc.relation.ispartof 11th International LISA Symposium, September 5-9 2016, Zurich, Zwitzerland
dc.relation.ispartofseries Journal of Physics: Conference Series 840 (2017), Nr. 1
dc.rights CC BY 3.0
dc.rights.uri https://creativecommons.org/licenses/by/3.0/
dc.subject Heterodyning eng
dc.subject Space probes eng
dc.subject Units of measurement eng
dc.subject Flight experiments eng
dc.subject Gravitational-wave observatory eng
dc.subject Heterodyne frequencies eng
dc.subject Heterodyne interferometry eng
dc.subject Interferometric measurement eng
dc.subject Length measurement eng
dc.subject Performance requirements eng
dc.subject Relative intensity noise eng
dc.subject Interferometry eng
dc.subject Gravitationswelle ger
dc.subject.ddc 530 | Physik ger
dc.title Coupling of relative intensity noise and pathlength noise to the length measurement in the optical metrology system of LISA Pathfinder
dc.type article
dc.type conferenceObject
dc.type Text
dc.relation.issn 1742-6588
dc.relation.doi https://doi.org/10.1088/1742-6596/840/1/012003
dc.bibliographicCitation.issue 1
dc.bibliographicCitation.volume 840
dc.bibliographicCitation.firstPage 12003
dc.description.version publishedVersion
tib.accessRights frei zug�nglich


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