First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds

Creators: Abbott, B.; Drever, R. W. P.; Brown, D. A.; Savov, P.; Siemens, X.; Thorne, K. S.; Vallisneri, M.; Abbott, R.; Adhikari, Rana X.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brown, D. A.; Busby, D.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; Creighton, T. D.; D'Ambrosio, E.; DeSalvo, R.; Dupuis, R. J.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Fairhurst, S.; Fazi, D.; Goggin, L.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Mandic, V.; Maros, E.; Marx, J. N.; Meshkov, S.; Messaritaki, E.; Meyers, D.; Miyakawa, O.; Nash, T.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Siemens, X.; Smith, M. R.; Sutton, P. J.; Tarallo, M.; Taylor, R.; Tyler, W.; Varvella, M.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Webber, D.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.; LIGO Scientific Collaboration; ALLEGRO Collaboration

Abstract

Data from the LIGO Livingston interferometer and the ALLEGRO resonant-bar detector, taken during LIGO's fourth science run, were examined for cross correlations indicative of a stochastic gravitational-wave background in the frequency range 850–950 Hz, with most of the sensitivity arising between 905 and 925 Hz. ALLEGRO was operated in three different orientations during the experiment to modulate the relative sign of gravitational-wave and environmental correlations. No statistically significant correlations were seen in any of the orientations, and the results were used to set a Bayesian 90% confidence level upper limit of Ω_(gw)(f)≤1.02, which corresponds to a gravitational-wave strain at 915 Hz of 1.5×10^(−23) Hz^(−1/2). In the traditional units of h^2_(100)Ω_(gw)(f), this is a limit of 0.53, 2 orders of magnitude better than the previous direct limit at these frequencies. The method was also validated with successful extraction of simulated signals injected in hardware and software.

Additional Information

© 2007 The American Physical Society. Received 28 March 2007; published 9 July 2007; publisher error corrected 23 July 2007. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sciences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Educacion y Ciencia, The National Aeronautics and Space Administration, the John Simon Guggenheim Foundation, the Alexander von Humboldt Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. The ALLEGRO observatory is supported by the National Science Foundation, Grant No. PHY0215479. This paper has been assigned LIGO Document No. LIGO-P050020-09-Z.

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