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First search for a stochastic gravitational-wave background from ultralight bosons

Tsukada, Leo and Callister, Thomas and Matas, Andrew and Meyers, Patrick (2019) First search for a stochastic gravitational-wave background from ultralight bosons. Physical Review D, 99 (10). Art. No. 103015. ISSN 2470-0010. doi:10.1103/physrevd.99.103015.

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Ultralight bosons with masses in the range 10^(−13)  eV ≤ m_b ≤ 10^(−12)  eV can induce a superradiant instability around spinning black holes (BHs) with masses of order 10−100  M⊙. This instability leads to the formation of a rotating “bosonic cloud” around the BH, which can emit gravitational waves (GWs) in the frequency band probed by ground-based detectors. The superposition of GWs from all such systems can generate a stochastic gravitational-wave background (SGWB). In this work, we develop a Bayesian data analysis framework to study the SGWB from bosonic clouds using data from Advanced LIGO and Advanced Virgo, building on previous work by Brito et al. [Phys. Rev. D 96, 064050 (2017)]. We further improve this model by adding a BH population of binary merger remnants. To assess the performance of our pipeline, we quantify the range of boson masses that can be constrained by Advanced LIGO and Advanced Virgo measurements at design sensitivity. Furthermore, we explore our capability to distinguish an ultralight boson SGWB from a stochastic signal due to distant compact binary coalescences (CBC). Finally, we present results of a search for the SGWB from bosonic clouds using data from Advanced LIGO’s first observing run. We find no evidence of such a signal. Due to degeneracies between the boson mass and unknown astrophysical quantities such as the distribution of isolated BH spins, our analysis cannot robustly exclude the presence of a bosonic field at any mass. Nevertheless, we show that under optimistic assumptions about the BH formation rate and spin distribution, boson masses in the range 2.0×10^(−13)  eV ≤ m_b ≤ 3.8×10^(−13)  eV are excluded at 95% credibility, although with less optimistic spin distributions, no masses can be excluded. The framework established here can be used to learn about the nature of fundamental bosonic fields with future gravitational wave observations.

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URLURL TypeDescription Paper
Callister, Thomas0000-0001-9892-177X
Additional Information:© 2019 American Physical Society. Received 21 January 2019; published 24 May 2019. We thank Richard Brito and Irina Dvorkin for their fruitful discussion and comments. L.T is supported by Japan Society for the Promotion of Science KAKENHI Grant No. JP18J21709. Laser Interferometer Gravitational Observatory (LIGO) was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement No. PHY-0757058. A.M and P.M are supported by NSF Grant No. PHY1505870. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through Project No. CE170100004. This paper carries LIGO Document Number LIGO-P1800232.
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)JP18J21709
Australian Research CouncilCE170100004
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Other Numbering System NameOther Numbering System ID
LIGO DocumentLIGO-P1800232
Issue or Number:10
Record Number:CaltechAUTHORS:20190603-145047199
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96047
Deposited By: Tony Diaz
Deposited On:03 Jun 2019 21:56
Last Modified:16 Nov 2021 17:17

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