Abstract

The output power of a cw Nd:YAG laser was stabilized in a dc-coupled feedback loop with a low-noise multiphotodiode detector and an electro-optic amplitude modulator in the frequency band from 1 Hz to 1 kHz. For the first time, to our knowledge, an independently measured relative power noise of 2.4×109Hz1/2 at 10 Hz was achieved, fulfilling the power stability requirements of the Advanced LIGO (Laser Interferometer Gravitational-Wave Observatory) gravitational wave detector.

© 2009 Optical Society of America

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K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D 73, 122005 (2006).
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Danzmann, K.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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Fritschel, P.

P. Fritschel, Proc. SPIE 4856, 282 (2003).
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Grote, H.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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Gustafson, E.

Heurs, M.

Hewitson, M.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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Hild, S.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
[CrossRef]

Hough, J.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
[CrossRef]

O. Jennrich, G. Newton, K. D. Skeldon, and J. Hough, Opt. Commun. 205, 405 (2002).
[CrossRef]

S. Rowan and J. Hough, Living Rev. Relativ. 3 (2000).

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O. Jennrich, G. Newton, K. D. Skeldon, and J. Hough, Opt. Commun. 205, 405 (2002).
[CrossRef]

Kawamura, S.

K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D 73, 122005 (2006).
[CrossRef]

Killow, C. J.

B. W. Barr, K. A. Strain, and C. J. Killow, Class. Quantum Grav. 22, 4279 (2005).
[CrossRef]

King, P. J.

Kwee, P.

Lück, H.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D 73, 122005 (2006).
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O. Jennrich, G. Newton, K. D. Skeldon, and J. Hough, Opt. Commun. 205, 405 (2002).
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Ottaway, D.

Prijatelj, M.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
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S. Rowan and J. Hough, Living Rev. Relativ. 3 (2000).

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P. R. Saulson, Fundamentals of Interferometric Gravitational Wave Detectors (World Scientific, 1994).
[CrossRef]

Savage, R. L.

Seel, S. U.

Seifert, F.

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O. Jennrich, G. Newton, K. D. Skeldon, and J. Hough, Opt. Commun. 205, 405 (2002).
[CrossRef]

Smith, J. R.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
[CrossRef]

Somiya, K.

K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D 73, 122005 (2006).
[CrossRef]

Strain, K. A.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
[CrossRef]

B. W. Barr, K. A. Strain, and C. J. Killow, Class. Quantum Grav. 22, 4279 (2005).
[CrossRef]

Ueda, K.

Uehara, N.

Weiss, R.

Willke, B.

Zucker, M.

Class. Quantum Grav.

S. Hild, H. Grote, J. Degallaix, S. Chelkowski, K. Danzmann, A. Freise, M. Hewitson, J. Hough, H. Lück, M. Prijatelj, K. A. Strain, J. R. Smith, and B. Willke, Class. Quantum Grav. 26, 055012 (2009).
[CrossRef]

B. W. Barr, K. A. Strain, and C. J. Killow, Class. Quantum Grav. 22, 4279 (2005).
[CrossRef]

Living Rev. Relativ.

S. Rowan and J. Hough, Living Rev. Relativ. 3 (2000).

Opt. Commun.

O. Jennrich, G. Newton, K. D. Skeldon, and J. Hough, Opt. Commun. 205, 405 (2002).
[CrossRef]

Opt. Lett.

Phys. Rev. D

K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D 73, 122005 (2006).
[CrossRef]

Proc. SPIE

P. Fritschel, Proc. SPIE 4856, 282 (2003).
[CrossRef]

Other

P. R. Saulson, Fundamentals of Interferometric Gravitational Wave Detectors (World Scientific, 1994).
[CrossRef]

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Figures (3)

Fig. 1
Fig. 1

Experimental setup. The laser (NPRO) was locked to the mode cleaner (MC) inside a pressure-tight tank. Power fluctuations were measured with four in-loop (IL) photodiodes to stabilize the laser power using an EOAM. The OOL detector was used to independently measure the power stability achieved. EOM, electro-optic phase modulator; FI, Faraday isolator; PBS, polarizing beam splitter; TIA, transimpedance amplifier; REF, voltage reference; λ / 2 , λ / 4 , wave plates.

Fig. 2
Fig. 2

Simplified schematic of the photodiode readout electronics.

Fig. 3
Fig. 3

OOL measured power noise. For low frequencies the measurement was limited by electronic noise and for frequencies above 7 Hz by shot noise of the IL (200 mA photocurrent) and OOL (189 mA photocurrent) detectors. The Advanced LIGO power noise requirement, shifted by 3 dB in the plot to account for the noise of the OOL detector, was met in the whole frequency band.

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