Abstract

Fluctuations in the position or propagation direction of the laser beam (beam jitter) is one of the most critical technical noise sources in an interferometric gravitational wave detector. These fluctuations couple to spurious misalignments of the mirrors forming the interferometer and potentially decrease the sensitivity. In this paper we calculate the transfer function of beam jitter into the gravitational wave channel for the Advanced LIGO detector and derive a first expression for the requirements on beam jitter for Advanced LIGO.

© 2005 Optical Society of America

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  1. B. Abbott et al., �??Detector description and performance for the first coincidence observations between LIGO and GEO,�?? Nucl. Instr. and Meth. in Phys. Res. A 517 (2004) 154-179. See also: <a href="http://www.ligo.caltech.edu">http://www.ligo.caltech.edu</a>
  2. Advanced LIGO is the first major upgrade of the current LIGO detectors. Informations about the planned upgrade are available at: <a href="http://www.ligo.caltech.edu/advLIGO/">http://www.ligo.caltech.edu/advLIGO/</a>
  3. Nergis Mavalvala, David Shoemaker, Daniel Sigg, �??Experimental Test of an Alignment-Sensing Scheme for a Gravitational-Wave Interferometer,�?? Applied Optics, 37 (1998) 7743
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  7. A. Siegman, Lasers (University Science, Sausalito, Calif. 1986)
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  10. N.A. Robertson et al., �??Seismic isolation and suspension systems for Advanced LIGO,�?? in Gravitational Wave and Particle Astrophysics Detectors, Proc. of SPIE, Vol. 5500, ed. James Hough, Gary Sanders (2004) 81-91
  11. This sensitivity curve was calculated using Bench. Informations about Bench is available at: <a href="http://cosmos.nirvana.phys.psu.edu/.">http://cosmos.nirvana.phys.psu.edu/</a> Details of the sensitivity curve depend on the fine-tuning of several parameters like tuning of the signal recycling mirror position, reflectivity of the mirrors, and the internal damping coefficients of the eigenmodes of the substrates and suspension systems. However, the sensitivity will not change by more than a factor of two at any signal frequency. The requirements for technical noise sources like beam jitter will not change significantly.
  12. The transfer function of the signal amplitude with respect to the displacement was calculated with Finesse. Finesse is an optical modeling program written by Andreas Freise. Finesse is available at <a href="http://www.rzg.mpg.de/�?adf/.">http://www.rzg.mpg.de/�?adf/.</a>
  13. S. Yoshida, G. Mueller, T. Delker, Q. Shu, D. Reitze, D.B. Tanner, J. Camp, J. Heefner, B. Kells, N. Mavalvala, D. Ouimette, H. Rong, R. Adhikari, P. Fritschel, M. Zucker, D. Sigg, �??Recent development in the LIGO Input Optics,�?? in �??Gravitational Wave Detection II,�?? Eds. S. Kawamura, N. Mio Proc. of the 2nd Tama International workshop on Gravitational wave Detection p. 51-59, Universal Academy Press, Tokyo, Japan Tokyo, Japan, October 19-22, 1999

Appl. Opt.

Applied Optics

Nergis Mavalvala, David Shoemaker, Daniel Sigg, �??Experimental Test of an Alignment-Sensing Scheme for a Gravitational-Wave Interferometer,�?? Applied Optics, 37 (1998) 7743

J. Opt. Soc. Am. A

J. Opt. Soc. Am. B

N. Mio Proc.

S. Yoshida, G. Mueller, T. Delker, Q. Shu, D. Reitze, D.B. Tanner, J. Camp, J. Heefner, B. Kells, N. Mavalvala, D. Ouimette, H. Rong, R. Adhikari, P. Fritschel, M. Zucker, D. Sigg, �??Recent development in the LIGO Input Optics,�?? in �??Gravitational Wave Detection II,�?? Eds. S. Kawamura, N. Mio Proc. of the 2nd Tama International workshop on Gravitational wave Detection p. 51-59, Universal Academy Press, Tokyo, Japan Tokyo, Japan, October 19-22, 1999

Nucl. Instr. and Meth. in Phys. Res. A

B. Abbott et al., �??Detector description and performance for the first coincidence observations between LIGO and GEO,�?? Nucl. Instr. and Meth. in Phys. Res. A 517 (2004) 154-179. See also: <a href="http://www.ligo.caltech.edu">http://www.ligo.caltech.edu</a>

Proc. of SPIE

N.A. Robertson et al., �??Seismic isolation and suspension systems for Advanced LIGO,�?? in Gravitational Wave and Particle Astrophysics Detectors, Proc. of SPIE, Vol. 5500, ed. James Hough, Gary Sanders (2004) 81-91

Other

This sensitivity curve was calculated using Bench. Informations about Bench is available at: <a href="http://cosmos.nirvana.phys.psu.edu/.">http://cosmos.nirvana.phys.psu.edu/</a> Details of the sensitivity curve depend on the fine-tuning of several parameters like tuning of the signal recycling mirror position, reflectivity of the mirrors, and the internal damping coefficients of the eigenmodes of the substrates and suspension systems. However, the sensitivity will not change by more than a factor of two at any signal frequency. The requirements for technical noise sources like beam jitter will not change significantly.

The transfer function of the signal amplitude with respect to the displacement was calculated with Finesse. Finesse is an optical modeling program written by Andreas Freise. Finesse is available at <a href="http://www.rzg.mpg.de/�?adf/.">http://www.rzg.mpg.de/�?adf/.</a>

Advanced LIGO is the first major upgrade of the current LIGO detectors. Informations about the planned upgrade are available at: <a href="http://www.ligo.caltech.edu/advLIGO/">http://www.ligo.caltech.edu/advLIGO/</a>

A. Siegman, Lasers (University Science, Sausalito, Calif. 1986)

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