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

Leo Tsukada1,2,*, Thomas Callister3, Andrew Matas4,5, and Patrick Meyers4,6

  • 1Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
  • 2Department of Physics, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
  • 3LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
  • 4School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
  • 5Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany
  • 6OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia

  • *tsukada@resceu.s.u-tokyo.ac.jp
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Phys. Rev. D 99, 103015 – Published 24 May, 2019

DOI: https://doi.org/10.1103/PhysRevD.99.103015

Abstract

Ultralight bosons with masses in the range 10−13  eV≤mb≤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≤mb≤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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Phys. Rev. D 99, 103015– Published 24 May, 2019
  • Received 21 January 2019
Article part of CHORUS
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