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  Einstein@Home all-sky search for continuous gravitational waves in LIGO O2 public data

Steltner, B., Papa, M. A., Eggenstein, H.-B., Allen, B., Dergachev, V., Prix, R., et al. (2021). Einstein@Home all-sky search for continuous gravitational waves in LIGO O2 public data. The Astrophysical Journal, 909(1): 79. doi:1038.47/1538-4357/abc7c9.

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 Creators:
Steltner, B.1, Author              
Papa, M. A.1, Author              
Eggenstein, H.-B.1, Author              
Allen, B.2, Author              
Dergachev, V.1, Author              
Prix, R.1, Author              
Machenschalk, B.1, Author              
Walsh , S., Author
Zhu , S. J., Author
Kwang, S., Author
Affiliations:
1Searching for Continuous Gravitational Waves, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2630691              
2Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Abstract: We conduct an all-sky search for continuous gravitational waves in the LIGO O2 data from the Hanford and Livingston detectors. We search for nearly-monochromatic signals with frequency between 20.0 Hz and 585.15 Hz and spin-down between -2.6e-9 Hz/s and 2.6e-10 Hz/s. We deploy the search on the Einstein@Home volunteer-computing project and follow-up the waveforms associated with the most significant results with eight further search-stages, reaching the best sensitivity ever achieved by an all-sky survey up to 500 Hz. Six of the inspected waveforms pass all the stages but they are all associated with hardware-injections, which are fake signals simulated at the LIGO detector for validation purposes. We recover all these fake signals with consistent parameters. No other waveform survives, so we find no evidence of a continuous gravitational wave signal at the detectability level of our search. We constrain the h0 amplitude of continuous gravitational waves at the detector as a function of the signal frequency, in half-Hz bins. The most constraining upper limit at 163.0 Hz is h0 = 1.3e25, at the 90% confidence level. Our results exclude neutron stars rotating faster than 5 ms with equatorial ellipticities larger than 1e-7 closer than 100 pc. These are deformations that neutron star crusts could easily support, according to some models.

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 Dates: 2020-09-252020-11-052021
 Publication Status: Published in print
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 Identifiers: arXiv: 2009.12260
DOI: 1038.47/1538-4357/abc7c9
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Title: The Astrophysical Journal
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Pages: - Volume / Issue: 909 (1) Sequence Number: 79 Start / End Page: - Identifier: -