Lasers for LISA: Overview and phase characteristics

Tröbs, Michael; Barke, Simon; Möbius, J.; Engelbrecht, Martin; Kracht, Dietmar; D'Arcio, Luigi; Heinzel, Gerhard; Danzmann, K.

doi:10.1088/1742-6596/154/1/012016

Cited by 12 publications

(10 citation statements)

References 9 publications

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“…The laser is based on a master oscillator power amplifier (MOPA) design with a seed laser as MO and a fiber amplifier as PA. We investigate an extended cavity diode laser (ECDL) with resonant optical feedback by an external cavity as a seed laser and a semiconductor optical amplifier (SOA) providing an optical output power out of the fiber of 300 mW (with 50% derating); see Section a. Various laser types have been investigated as a seed laser source for LISA [3,4]. To date a nonplanar ring oscillator (NPRO) is the baseline for the LISA seed laser.…”

Section: Laser Designmentioning

confidence: 99%

A new laser technology for LISA

Dahl

Cebeci

Fitzau

et al. 2019

International Conference on Space Optics — ICSO 2018

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Within the European Space Agency (ESA) activity "Gravitational Wave Observatory Metrology Laser" we designed a laser head to fulfill the LISA laser requirements using a non-NPRO seed laser technology: an external cavity diode laser (ECDL) with resonant optical feedback from an external cavity as master oscillator for further linewidth narrowing. Furthermore, our design features a single-stage fiber amplifier with an amplification factor of about 20 dB. This paper covers the requirements on the laser source for LISA, the design and first results of performance characterization of the laser head breadboard.

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Section: Laser Designmentioning

confidence: 99%

A new laser technology for LISA

Dahl

Cebeci

Fitzau

et al. 2019

International Conference on Space Optics — ICSO 2018

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“…The long time-scale fluctuations can be corrected by changing the laser crystal temperature and the short ones by squeezing the YAG crystal. Lasers, with similar characteristics, suitable for the LISA mission have already been investigated [16] and are actually, to our knowledge, in technology readiness level (TRL) 4-6 [17].…”

Section: Methodsmentioning

confidence: 99%

Molecular laser stabilization at low frequencies for the LISA mission

et al. 2010

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We have developed a 532 nm iodine stabilized laser system that may be suitable for the LISA mission (Laser Interferometer Space Antenna) or other future spaceborne missions. This system is based on an externally frequency-doubled Nd:YAG laser source and uses the molecular transfer spectroscopy technique for the frequency stabilization. This technique has been optimized for LISA: compactness (less than 1.1×1.1m2), vacuum compatibility, ease of use and initialization, minimization of the number of active components (acousto-optic modulators are both used for frequency shifting and phase modulating the pump beam). By locking on the a10 hyperfine component of the R(56)32-0 transition, we find an Allan standard deviation (σ) of 3×10-14 at 1 s and σ<2×10-14 for 20s≤τ≤103s. In terms of linear spectral density, this roughly corresponds to a stability better than 30Hz/Hz between 10-2 and 1 Hz with a stability decrease close to 1/f below 10 mHz

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“…Fluctuations in the laser power relative to the average absolute power level, the so-called relative intensity noise (RIN), will directly couple to the photocurrent of the receiving photo detector as one part of the read-out noise and deteriorate the interferometric length measurements. [27]. Below this frequency the noise increases significantly so that no measurements at heterodyne frequencies below 5 MHz are possible.…”

Section: Lasers Optics and Photoreceiversmentioning

confidence: 99%

Towards a gravitational wave observatory designer: sensitivity limits of spaceborne detectors

Barke

Wang

Delgado

et al. 2015

Class. Quantum Grav.

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The most promising concept for low frequency (millihertz to hertz) gravitational wave observatories are laser interferometric detectors in space. It is usually assumed that the noise floor for such a detector is dominated by optical shot noise in the signal readout. For this to be true, a careful balance of mission parameters is crucial to keep all other parasitic disturbances below shot noise. We developed a web application that uses over 30 input parameters and considers many important technical noise sources and noise suppression techniques to derive a realistic position noise budget. It optimizes free parameters automatically and generates a detailed report on all individual noise contributions. Thus one can easily explore the entire parameter space and design a realistic gravitational wave observatory. In this document we describe the different parameters, present all underlying calculations, and compare the final observatory's sensitivity with astrophysical sources of gravitational waves. We use as an example parameters currently assumed to be likely applied to a space mission proposed to be launched in 2034 by the European Space Agency. The web application itself is publicly available on the Internet at http://spacegravity.org/designer. Future versions of the web application will Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. incorporate the frequency dependence of different noise sources and include a more detailed model of the observatory's residual acceleration noise.

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Lasers for LISA: Overview and phase characteristics

Cited by 12 publications

References 9 publications

A new laser technology for LISA

A new laser technology for LISA

Molecular laser stabilization at low frequencies for the LISA mission

Towards a gravitational wave observatory designer: sensitivity limits of spaceborne detectors

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