Authors

J. Aasi, California Institute of TechnologyFollow
B. P. Abbott, California Institute of TechnologyFollow
R. Abbott, California Institute of TechnologyFollow
T. Abbott, Louisiana State UniversityFollow
M. R. Abernathy, California Institute of TechnologyFollow
F. Acernese, Università degli Studi di SalernoFollow
K. Ackley, University of FloridaFollow
C. Adams, LIGO LivingstonFollow
T. Adams, Cardiff UniversityFollow
P. Addesso, Università degli Studi del SannioFollow
R. X. Adhikari, California Institute of TechnologyFollow
V. Adya, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)Follow
C. Affeldt, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)Follow
M. Agathos, FOM-Institute of Subatomic Physics - NIKHEFFollow
K. Agatsuma, FOM-Institute of Subatomic Physics - NIKHEFFollow
N. Aggarwal, LIGO, Massachusetts Institute of TechnologyFollow
O. D. Aguiar, Instituto Nacional de Pesquisas EspaciaisFollow
A. Ain, Inter-University Centre for Astronomy and Astrophysics IndiaFollow
P. Ajith, Tata Institute of Fundamental Research, MumbaiFollow
A. Alemic, Syracuse University
B. Allen, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)Follow
A. Allocca, Università degli Studi di SienaFollow
D. Amariutei, University of FloridaFollow
S. B. Anderson, California Institute of TechnologyFollow
W. G. Anderson, University of Wisconsin-MilwaukeeFollow
K. Arai, California Institute of Technology
M. C. Araya, California Institute of Technology
C. Arceneaux, University of Mississippi
J. S. Areeda, California State University, Fullerton
S. Ast, Gottfried Wilhelm Leibniz Universität Hannover
S. M. Aston, LIGO Livingston
P. Astone, Istituto Nazionale di Fisica Nucleare - INFN
P. Aufmuth, Gottfried Wilhelm Leibniz Universität Hannover

Document Type

Article

Publication Date

11-1-2015

Abstract

We describe directed searches for continuous gravitational waves (GWs) in data from the sixth Laser Interferometer Gravitational-wave Observatory (LIGO) science data run. The targets were nine young supernova remnants not associated with pulsars; eight of the remnants are associated with non-pulsing suspected neutron stars. One target's parameters are uncertain enough to warrant two searches, for a total of 10. Each search covered a broad band of frequencies and first and second frequency derivatives for a fixed sky direction. The searches coherently integrated data from the two LIGO interferometers over time spans from 5.3-25.3 days using the matched-filtering -statistic. We found no evidence of GW signals. We set 95% confidence upper limits as strong (low) as 4 × 10-25 on intrinsic strain, 2 × 10-7 on fiducial ellipticity, and 4 × 10-5 on r-mode amplitude. These beat the indirect limits from energy conservation and are within the range of theoretical predictions for neutron-star ellipticities and r-mode amplitudes.

Publication Source (Journal or Book title)

Astrophysical Journal

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