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Stochastic gravitational wave background originating from halo mergers

Takahiro Inagaki1,*, Keitaro Takahashi2,1, and Naoshi Sugiyama1,3,4

  • 1Department of Physics and Astrophysics, Nagoya University, Nagoya 464-8602, Japan
  • 2Faculty of Science, Kumamoto University, 2-39-1, Kurokami, Kumamoto 860-8555, Japan
  • 3Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Kashiwa, Chiba, 277-8568, Japan
  • 4Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya 464-8602, Japan

  • *inagaki@a.phys.nagoya-u.ac.jp
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Phys. Rev. D 85, 104051 – Published 29 May, 2012

DOI: https://doi.org/10.1103/PhysRevD.85.104051

Abstract

The stochastic gravitational wave background (GWB) from halo mergers is investigated by a quasianalytic method. The method we employ consists of two steps. The first step is to construct a merger tree by using the extended Press-Schechter formalism or the Sheth & Tormen formalism, with Monte Carlo realizations. This merger tree provides evolution of halo masses. From N-body simulation of two-halo mergers, we can estimate the amount of gravitational wave emission induced by the individual merger process. Therefore, the second step is to combine this gravitational wave emission with the merger tree and obtain the amplitude of the GWB. We find ΩGW∼10−19 for f∼10−17–10−16  Hz, where ΩGW is the energy density of the GWB. It turns out that most of the contribution on the GWB comes from halos with masses below 1015M⊙ and mergers at low redshift, i.e., 0<z<0.8.

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References (16)

  1. K. Sato, Mon. Not. R. Astron. Soc. 195, 467 (1981).
  2. A. H. Guth, Phys. Rev. D 23, 347 (1981).
  3. A. Albrecht and P. J. Steinhardt, Phys. Rev. Lett. 48, 1220 (1982).
  4. A. D. Linde, Phys. Lett. 108B, 389 (1982).
  5. S. Kuroyanagi, T. Chiba, and N. Sugiyama, Phys. Rev. D 79, 103501 (2009).
  6. S. Mollerach, D. Harari, and S. Matarrese, Phys. Rev. D 69, 063002 (2004).
  7. K. N. Ananda, C. Clarkson, and D. Wands, Phys. Rev. D 75, 123518 (2007).
  8. D. Baumann, P. Steinhardt, K. Takahashi, and K. Ichiki, Phys. Rev. D 76, 084019 (2007).
  9. J. R. Pritchard and M. Kamionkowski, Ann. Phys. (N.Y.) 318, 2 (2005).
  10. C. Lacey and S. Cole, Mon. Not. R. Astron. Soc. 262, 627 (1993).
  11. C. Lacey and S. Cole, Mon. Not. R. Astron. Soc. 271, 676 (1994).
  12. T. Inagaki, K. Takahashi, S. Masaki, and N. Sugiyama, Phys. Rev. D 82, 124007 (2010).
  13. E. Komatsu, K. M. Smith, J. Dunkley, C. L. Bennett, B. Gold, G. Hinshaw, N. Jarosik, D. Larson, M. R. Nolta, L. Page et al., Astrophys. J. Suppl. Ser. 192, 18 (2011).
  14. R. S. Somerville and T. S. Kolatt, Mon. Not. R. Astron. Soc. 305, 1 (1999).
  15. R. K. Sheth and G. Tormen, Mon. Not. R. Astron. Soc. 308, 119 (1999).
  16. A. Jenkins, C. S. Frenk, S. D. M. White, J. M. Colberg, S. Cole, A. E. Evrard, H. M. P. Couchman, and N. Yoshida, Mon. Not. R. Astron. Soc. 321, 372 (2001).

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Phys. Rev. D 85, 104051– Published 29 May, 2012
  • Received 9 February 2012

© 2012 American Physical Society

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