Beam jitter coupling in advanced LIGO

Optics Express

Volumn 13, Issue 18, 2005, Pages 7118-7132

  Mueller, Guido ^a  

^a Department of Physics University of Florida ^*  (United States)

Author keywords

[No Author keywords available]

Indexed keywords

GRAVITATION; INTERFEROMETERS; LASER BEAMS; MIRRORS; WAVE EFFECTS; WAVE PROPAGATION;

BEAM JITTER; SPURIOUS MISALIGNMENTS; TECHNICAL NOISE; TRANSFER FUNCTION;

JITTER;

EID: 24944543304     PISSN: 10944087     EISSN: 10944087     Source Type: Journal    
DOI: 10.1364/OPEX.13.007118     Document Type: Article

References (13)

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: www.ligo.caltech.edu
2. Advanced LIGO is the first major upgrade of the current LIGO detectors. Informations about the planned upgrade are available at: http://www.ligo. caltech.edu/advLIGO/
3. Nergis Mavalvala, David Shoemaker, Daniel Sigg, "Experimental Test of an Alignment-Sensing Scheme for a Gravitational-Wave Interferometer," Applied Optics, 37 (1998) 7743
4. Peter Fritschel, Nergis Mavalvala, David Shoemaker, Daniels Sigg, Michael Zucker, Gabriela Gonzales, "Alignment of an interferometric gravitational wave detector," Appl. Opt., 37 (1998) 6734
5. Kenneth Strain et al., "Sensing and control in dual-recycled laser interferometer gravitational-wave detectors," Appl. Opt., 42 (2003) 1244
6. Guido Mueller et al., "Dual-recycled cavity-enhanced Michelson interferometer for gravitational-wave detection," Appl. Opt., 42 (2003) 1257
7. A. Siegman, Lasers (University Science, Sausalito, Calif. 1986)
8. Y. Hefetz, N. Mavalvala, and D. Sigg, "Principles of calculating alignment signals in complex optical interferometers," J. Opt. Soc. Am. B14 (1997) 1597
9. D. Sigg, N. Mavalvala, "Principles of calculating the dynamical response of misaligned complex resonant optical interferometers," J. Opt. Soc. Am. A17 (2000) 1642
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: http://cosmos.nirvana.phys.psu.edu/~lsf/Benchmarks/main. html. 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 http://www.rzg.mpg.de/adf/.
13. S. Yoshida, G. Mueller, T. Delker, Q. Shu, D. Reitze, D.B. Tanner, J. Camp, J. Heefner, B. Keils, 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