Upper limits on a stochastic background of gravitational waves

Authors

B. Abbott, California Institute of Technology
R. Abbott, California Institute of Technology
R. Adhikari, California Institute of Technology
J. Agresti, California Institute of Technology
P. Ajith, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
B. Allen, University of Wisconsin-Milwaukee
J. Allen, Massachusetts Institute of Technology
R. Amin, Louisiana State University
S. B. Anderson, California Institute of Technology
W. G. Anderson, University of Wisconsin-Milwaukee
M. Araya, California Institute of Technology
H. Armandula, California Institute of Technology
M. Ashley, Pennsylvania State University
C. Aulbert, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
S. Babak, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
R. Balasubramanian, Cardiff University
S. Ballmer, Massachusetts Institute of Technology
B. C. Barish, California Institute of Technology
C. Barker, LIGO Hanford
D. Barker, LIGO Hanford
M. A. Barton, California Institute of Technology
K. Bayer, Massachusetts Institute of Technology
K. Belczynski, Northwestern University
J. Betzwieser, Massachusetts Institute of Technology
B. Bhawal, California Institute of Technology
I. A. Bilenko, Lomonosov Moscow State University
G. Billingsley, California Institute of Technology
E. Black, California Institute of Technology
K. Blackburn, California Institute of Technology
L. Blackburn, Massachusetts Institute of Technology
B. Bland, LIGO Hanford
L. Bogue, LIGO Livingston
R. Bork, California Institute of Technology

Document Type

Article

Publication Date

11-25-2005

Abstract

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 0 < 8.4 × 10 -4 in the 69-156 Hz band is ∼10 5 times lower than the previous result in this frequency range. © 2005 The American Physical Society.

Publication Source (Journal or Book title)

Physical Review Letters

Recommended Citation

Abbott, B., Abbott, R., Adhikari, R., Agresti, J., Ajith, P., Allen, B., Allen, J., Amin, R., Anderson, S., Anderson, W., Araya, M., Armandula, H., Ashley, M., Aulbert, C., Babak, S., Balasubramanian, R., Ballmer, S., Barish, B., Barker, C., Barker, D., Barton, M., Bayer, K., Belczynski, K., Betzwieser, J., Bhawal, B., Bilenko, I., Billingsley, G., Black, E., Blackburn, K., Blackburn, L., Bland, B., Bogue, L., & Bork, R. (2005). Upper limits on a stochastic background of gravitational waves. Physical Review Letters, 95 (22) https://doi.org/10.1103/PhysRevLett.95.221101