Author ORCID Identifier

Chiadini, Francesco: 0000-0002-9339-8622
Shcheblanov, Nikita: 0000-0001-8696-2435
Christensen, Nelson: 0000-0002-6870-4202
Karki, Sudarshan: 0000-0001-9982-3661
Edy, Oliver: 0000-0001-9617-8724
Kuroyanagi, Sachiko: 0000-0001-6538-1447
Mondin, Marina: 0000-0003-3105-3802
Nakamura, Kouji: 0000-0001-6148-4289
Creighton, Jolien: 0000-0003-3600-2406
Carapella, Giovanni: 0000-0002-0095-1434
Asali, Yasmeen: 0000-0002-8320-2198
Nuttall, Laura Kate: 0000-0001-7472-0201
Williamson, Andrew: 0000-0002-7627-8688
Hollows, Ian: 0000-0002-3404-6459
Shinkai, Hisa-Aki: 0000-0003-1082-2844
Harry, Ian: 0000-0002-5304-9372
Kovalam, Manoj: 0000-0001-8143-9696
Charlton, Philip: 0000-0002-4263-2706
Farr, Ben: 0000-0002-2916-9200
Bassiri, Riccardo: 0000-0001-8171-6833
Pitkin, Matthew: 0000-0003-4548-526X
Nakano, Hiroyuki: 0000-0001-7665-0796
Lundgren, Andrew: 0000-0002-0363-4469
Martinez, Mario: 0000-0002-3135-945X
Mozzon, Simone: 0000-0002-8855-2509
Sanchis-Gual, Nicolas: 0000-0001-5375-7494

Document Type


Publication Date



We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0; +0.1] x 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 LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h(0) are similar to 1.7 x 10(-25) near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are similar to 6.3 x 10(-26). These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a populationaveraged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are similar to 1.4 x 10(-25). These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of similar to 2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.

Publication Source (Journal or Book title)

Physical Review D