Laser development for LISA

Tröbs, Michael; Weßels, P.; Fallnich, Carsten; Bode, M.; Freitag, Ingo; Skorupka, Sascha; Heinzel, Gerhard; Danzmann, Karsten

doi:10.1088/0264-9381/23/8/S20

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Laser development for LISA

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Tröbs, Michael
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

Skorupka, Sascha
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;
AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Heinzel, Gerhard
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons40437

Danzmann, Karsten
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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cqg6_8_s20.pdf
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引用

Tröbs, M., Weßels, P., Fallnich, C., Bode, M., Freitag, I., Skorupka, S., Heinzel, G., & Danzmann, K. (2006). Laser development for LISA. Classical and Quantum Gravity, 23(8), S151-S158.

引用: https://hdl.handle.net/11858/00-001M-0000-0013-4C00-B

要旨

The two most promising configurations for the LISA laser are a stand-alone diode-pumped nonplanar ring oscillator (NPRO) or a fibre amplifier seeded by a low-power NPRO. The stand-alone laser was stabilized in frequency to a ULE cavity and in power to an electronic reference. For the first time the LISA requirement of relative power noise below 2 × 10-4/Hz1/2 was fulfilled in the whole frequency range from 0.1 mHz to 1 Hz. The LISA goal of frequency noise below 30 Hz/Hz1/2 was achieved for frequencies above 3 mHz. As a first step in the characterization of an oscillator-amplifier system, the excess frequency noise of an ytterbium-doped fibre amplifier was measured. For frequencies between 0.1 mHz and 1 Hz the excess noise was measured to be below 0.1 Hz/Hz1/2, which is significantly below the free-running frequency noise of NPROs.