B. P. Abbott, California Institute of Technology
R. Abbott, California Institute of Technology
T. D. Abbott, Louisiana State University
M. R. Abernathy, American University
F. Acernese, Università degli Studi di Salerno
K. Ackley, University of Florida
C. Adams, LIGO Livingston
T. Adams, Université Savoie Mont Blanc
P. Addesso, Università degli Studi del Sannio
R. X. Adhikari, California Institute of Technology
V. B. Adya, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
C. Affeldt, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
M. Agathos, FOM-Institute of Subatomic Physics - NIKHEF
K. Agatsuma, FOM-Institute of Subatomic Physics - NIKHEF
N. Aggarwal, LIGO, Massachusetts Institute of Technology
O. D. Aguiar, Instituto Nacional de Pesquisas Espaciais
L. Aiello, Istituto Nazionale di Fisica Nucleare - INFN
A. Ain, Inter-University Centre for Astronomy and Astrophysics India
P. Ajith, Tata Institute of Fundamental Research, Mumbai
B. Allen, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
A. Allocca, Università di Pisa
P. A. Altin, The Australian National University
S. B. Anderson, California Institute of Technology
W. G. Anderson, University of Wisconsin-Milwaukee
K. Arai, California Institute of Technology
M. C. Araya, California Institute of Technology
C. C. Arceneaux, University of Mississippi
J. S. Areeda, California State University, Fullerton
N. Arnaud, Laboratoire de l'Accélérateur Linéaire
K. G. Arun, Chennai Mathematical Institute
S. Ascenzi, Istituto Nazionale di Fisica Nucleare - INFN
G. Ashton, University of Southampton
M. Ast, Universität Hamburg

Document Type

Article

Publication Date

8-15-2016

Abstract

We report on a comprehensive all-sky search for periodic gravitational waves in the frequency band 100-1500 Hz and with a frequency time derivative in the range of [-1.18,+1.00]×10-8 Hz/s. Such a signal could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our galaxy. This search uses the data from the initial LIGO sixth science run and covers a larger parameter space with respect to any past search. A Loosely Coherent detection pipeline was applied to follow up weak outliers in both Gaussian (95% recovery rate) and non-Gaussian (75% recovery rate) bands. No gravitational wave signals were observed, and upper limits were placed on their strength. Our smallest upper limit on worst-case (linearly polarized) strain amplitude h0 is 9.7×10-25 near 169 Hz, while at the high end of our frequency range we achieve a worst-case upper limit of 5.5×10-24. Both cases refer to all sky locations and entire range of frequency derivative values.

Publication Source (Journal or Book title)

Physical Review D

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