Authors

J. Abadie, California Institute of Technology
B. P. Abbott, California Institute of Technology
R. Abbott, California Institute of Technology
M. Abernathy, University of Glasgow
T. Accadia, Université Savoie Mont Blanc
F. Acernese, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli
C. Adams, LIGO Livingston
R. Adhikari, California Institute of Technology
P. Ajith, California Institute of Technology
B. Allen, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
G. S. Allen, Stanford University
E. Amador Ceron, University of Wisconsin-Milwaukee
R. S. Amin, Louisiana State University
S. B. Anderson, California Institute of Technology
W. G. Anderson, University of Wisconsin-Milwaukee
F. Antonucci, Istituto Nazionale di Fisica Nucleare - INFN
M. A. Arain, University of Florida
M. C. Araya, California Institute of Technology
M. Aronsson, California Institute of Technology
K. G. Arun, Chennai Mathematical Institute
Y. Aso, California Institute of Technology
S. M. Aston, University of Birmingham
P. Astone, Istituto Nazionale di Fisica Nucleare - INFN
D. Atkinson, LIGO Hanford
P. Aufmuth, Gottfried Wilhelm Leibniz Universität Hannover
C. Aulbert, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
S. Babak, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
P. Baker, Montana State University
G. Ballardin, European Gravitational Observatory (EGO)
S. Ballmer, California Institute of Technology
D. Barker, LIGO Hanford
Tiffany Z. Summerscales, Andrews UniversityFollow

Document Type

Article

Publication Date

12-29-2011

Abstract

The gravitational-wave (GW) sky may include nearby pointlike sources as well as stochastic backgrounds. We perform two directional searches for persistent GWs using data from the LIGO S5 science run: one optimized for pointlike sources and one for arbitrary extended sources. Finding no evidence to support the detection of GWs, we present 90% confidence level (C.L.) upper-limit maps of GW strain power with typical values between 2-20×10-50strain2Hz-1 and 5-35×10 -49strain2Hz-1sr-1 for pointlike and extended sources, respectively. The latter result is the first of its kind. We also set 90% C.L. limits on the narrow-band root-mean-square GW strain from interesting targets including Sco X-1, SN 1987A and the Galactic center as low as 7×10-25 in the most sensitive frequency range near 160 Hz. © 2011 American Physical Society.

Journal Title

Physical Review Letters

Volume

107

Issue

27

DOI

https://doi.org/10.1103/PhysRevLett.107.271102

First Department

Physics

Acknowledgements

Retrieved January 29, 2021 from https://arxiv.org/pdf/1109.1809.pdf

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