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Detecting black-hole binary clustering via the second-generation gravitational-wave detectors

Toshiya Namikawa1,2, Atsushi Nishizawa3,4, and Atsushi Taruya5,6

  • 1Department of Physics, Stanford University, Stanford, California 94305, USA
  • 2Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, Menlo Park, California 94025, USA
  • 3Department of Physics and Astronomy, The University of Mississippi, University, Mississippi 38677, USA
  • 4Theoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USA
  • 5Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
  • 6Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Chiba 277-8583, Japan

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Phys. Rev. D 94, 024013 – Published 5 July, 2016

DOI: https://doi.org/10.1103/PhysRevD.94.024013

Abstract

The first discovery of the gravitational-wave (GW) event, GW150914, suggests a higher merger rate of black-hole (BH) binaries. If this is true, a number of BH binaries will be observed via the second-generation GW detectors, and the statistical properties of the observed BH binaries can be scrutinized. A naive but important question to ask is whether the spatial distribution of BH binaries faithfully traces the matter inhomogeneities in the Universe or not. Although the BH binaries are thought to be formed inside the galaxies in most of the scenarios, there is no observational evidence to confirm such a hypothesis. Here, we estimate how well the second-generation GW detectors can statistically confirm the BH binaries to be a tracer of the large-scale structure by looking at the auto- and cross-correlation of BH binaries with photometric galaxies and weak-lensing measurements, finding that, with a 3 year observation, the >3σ detection of a nonzero signal is possible if the BH merger rate today is n˙0≳100  Gpc−3 yr−1 and the clustering bias of BH binaries is bBH,0≳1.5.

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Phys. Rev. D 94, 024013– Published 5 July, 2016
  • Received 1 April 2016
Article part of CHORUS

© 2016 American Physical Society

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