Upper Limits on a Stochastic Background of Gravitational Waves

Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith, P.; Allen, B.; Allen, J.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Araya, M.; Armandula, H.; Ashley, M.; Aulbert, C.; Babak, S.; Balasubramanian, R.; Ballmer, S.; Barish, B. C.; Barker, C.; Barker, D.; Barton, M. A.; Bayer, K.; Belczynski, K.; Betzwieser, J.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Black, E.; Blackburn, K.; Blackburn, L.; Bland, B.; Bogue, L.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brown, D. A.; Buonanno, A.; Busby, D.; Butler, W. E.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cardenas, L.; Carter, K.; Casey, M. M.; Charlton, P.; Chatterji, S.; Chen, Y.; Chin, D.; Christensen, N.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Cook, D.; Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandar, S.; Díaz, M.; di Credico, A.; Drever, R. W. P.; Dupuis, R. J.; Ehrens, P.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Finn, L. S.; Franzen, K. Y.; Frey, R. E.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Ganezer, K. S.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Goda, K.; Goggin, L.; González, G.; Gray, C.; Gretarsson, A. M.; Grimmett, D.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R. et al.
Referencia bibliográfica

Physical Review Letters, vol. 95, Issue 22, id. 221101

Fecha de publicación:
11
2005
Número de autores
304
Número de autores del IAC
0
Número de citas
82
Número de citas referidas
68
Descripción
The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of Ω0<8.4×10-4 in the 69-156 Hz band is ˜105 times lower than the previous result in this frequency range.