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Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO--Virgo data

The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, Abbott, R., Abe, H., Acernese, F., et al. (in preparation). Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO--Virgo data.

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2204.04523.pdf (Preprint), 1017KB
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2204.04523.pdf
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### Creators

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Creators:
The LIGO Scientific Collaboration, Author
the Virgo Collaboration, Author
the KAGRA Collaboration, Author
Abbott, R., Author
Abe, H., Author
Acernese, F., Author
Ackley, K., Author
Affeldt, C.1, Author
Agarwal, D., Author
Agathos, M., Author
Agatsuma, K., Author
Aggarwal, N., Author
Aguiar, O. D., Author
Aiello, L., Author
Ain, A., Author
Ajith, P., Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24010
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290
3Multi-messenger Astrophysics of Compact Binaries, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_3329942
4Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
Abstract: We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO--Virgo run in the detector frequency band $[10,2000]\rm~Hz$ have been used. No significant detection was found and 95$\%$ confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about $7.6\times 10^{-26}$ at $\simeq 142\rm~Hz$. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass -- boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC.

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Dates: 2022-04-09
Publication Status: Not specified
Pages: 25 pages, 5 figures
Publishing info: -
Rev. Type: -
Identifiers: arXiv: 2204.04523
Degree: -

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