Abstract
We present the results of an all-sky search for continuous gravitational-wave signals with frequencies in the 500-1700Hz range targeting neutron stars with ellipticity of 10^{-8}. The search is done on LIGO O2 data using the Falcon analysis pipeline. The results presented here double the sensitivity over any other result on the same data [B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration), Phys. Rev. D 100, 024004 (2019)PRVDAQ2470-001010.1103/PhysRevD.100.024004, C. Palomba et al., Phys. Rev. Lett. 123, 171101 (2019)PRLTAO0031-900710.1103/PhysRevLett.123.171101]. The search is capable of detecting low-ellipticity sources up to 170pc. We establish strict upper limits which hold for worst-case signal parameters. We list outliers uncovered by the search, including several which we cannot associate with any known instrumental cause.
Highlights
We present the results of an all-sky search for continuous gravitational-wave signals with frequencies in the 500–1700 Hz range targeting neutron stars with ellipticity of 10−8
We establish strict upper limits which hold for worst-case signal parameters
Introduction.—Continuous gravitational waves are expected over a broad range of frequencies from rapidly rotating compact stars such as neutron stars due to a variety of mechanisms [1] as well as from more exotic scenarios [2,3,4,5,6,7]
Summary
We have explored the LIGO O1-run data employing the Falcon search with a first-stage coherence length of 4 h and demonstrated its performance and computational efficiency [10,13]. The last stage includes consistency checks between the single-instrument results Candidates that survive this entire sequence of tests represent one of the results of the search. Upper limit results.—The other results of this paper are the 95% confidence-level continuous gravitational-wave amplitude upper limits h0 These represent the smallest amplitude of a continuous signal with a given frequency, coming from an arbitrary direction in the sky and with frequency drift in our search range, that we can exclude from impinging on the detectors. We have assumed a quasimonochromatic signal with slow evolution in frequency that can be approximated by a quadratic model: fðtÞ 1⁄4 f0 þ ðt − t0Þf1 þ ðt − t0Þ2f2=2; ð1Þ
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