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Laser-interferometric detectors for gravitational wave backgrounds at 100 MHz: Detector design and sensitivity

Atsushi Nishizawa1,*, Seiji Kawamura2, Tomotada Akutsu3, Koji Arai2, Kazuhiro Yamamoto2, Daisuke Tatsumi2, Erina Nishida4, Masa-aki Sakagami1, Takeshi Chiba5 et al.

Ryuichi Takahashi6 and Naoshi Sugiyama6

  • 1Graduate School of Human and Environmental Studies, Kyoto University, Kyoto 606-8501, Japan
  • 2TAMA Project, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
  • 3Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
  • 4Ochanomizu University, Bunkyo-ku, Tokyo 112-8610, Japan
  • 5Department of Physics, College of Humanities and Sciences, Nihon University, Tokyo 156-8550, Japan
  • 6Graduate School of Science, Nagoya University, Nagoya 467-8602, Japan

  • *atsushi.nishizawa@nao.ac.jp
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Phys. Rev. D 77, 022002 – Published 28 January, 2008

DOI: https://doi.org/10.1103/PhysRevD.77.022002

Abstract

Recently, observational searches for gravitational wave background (GWB) have been developed and given direct and indirect constraints on the energy density of GWB in a broad range of frequencies. These constraints have already rejected some theoretical models of large GWB spectra. However, at 100 MHz, there is no strict upper limit from direct observation, though the indirect limit by He2 abundance due to big-bang nucleosynthesis exists. In this paper, we propose an experiment with laser interferometers searching GWB at 100 MHz. We considered three detector designs and evaluated the GW response functions of a single detector. As a result, we found that, at 100 MHz, the most sensitive detector is the design, a so-called synchronous recycling interferometer, which has better sensitivity than an ordinary Fabry-Perot Michelson interferometer by a factor of 3.3 at 100 MHz. When we select the arm length of 0.75 m and realistic optical parameters, the best sensitivity achievable is h≈7.8×10−21  Hz−1/2 at 100 MHz with bandwidth ∼2  kHz.

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References (32)

  1. P. J. E. Peebles and A. Vilenkin, Phys. Rev. D 59, 063505 (1999).
  2. M. Giovannini, Phys. Rev. D 60, 123511 (1999).
  3. M. Giovannini, Phys. Rev. D 58, 083504 (1998).
  4. A. Riazuelo and J. P. Uzan, Phys. Rev. D 62, 083506 (2000).
  5. H. Tashiro, T. Chiba, and M. Sasaki, Classical Quantum Gravity 21, 1761 (2004).
  6. R. Easther and E. A. Lim, J. Cosmol. Astropart. Phys. 04 (2006) 010.
  7. J. Garcia-Bellido and D. G. Figueroa, Phys. Rev. Lett. 98, 061302 (2007).
  8. J. Dufaux, A. Bergman, G. Felder, L. Kofman, and J. Uzan, Phys. Rev. D 76, 123517 (2007).
  9. M. Gasperini and M. Giovannini, Phys. Rev. D 47, 1519 (1993).
  10. R. Brustein, M. Gasperini, M. Giovannini, and G. Veneziano, Phys. Lett. B 361, 45 (1995).
  11. M. Gasperini and G. Veneziano, Phys. Rep. 373, 1 (2003).
  12. T. Nakamura, M. Sasaki, T. Tanaka, and K. S. Thorne, Astrophys. J. 487, L139 (1997).
  13. K. Ioka, T. Chiba, T. Tanaka, and T. Nakamura, Phys. Rev. D 58, 063003 (1998).
  14. G. S. Bisnovatyi-Kogan and V. N. Rudenko, Classical Quantum Gravity 21, 3347 (2004).
  15. S. S. Seahra, C. Clarkson, and R. Maartens, Phys. Rev. Lett. 94, 121302 (2005).
  16. C. Clarkson and S. S. Seahra, Classical Quantum Gravity 24, F33 (2007).
  17. T. L. Smith, M. Kamionkowski, and A. Cooray, Phys. Rev. D 73, 023504 (2006).
  18. F. A. Jenet et al., Astrophys. J. 653, 1571 (2006).
  19. J. W. Armstrong, L. Iess, P. Tortora, and B. Bertotti, Astrophys. J. 599, 806 (2003).
  20. B. Abbot et al., Astrophys. J. 659, 918 (2007).
  21. M. Maggiore, Phys. Rep. 331, 283 (2000).
  22. A. M. Cruise and R. M. J. Ingley, Classical Quantum Gravity 23, 6185 (2006).
  23. R. W. P. Drever, Gravitational Radiation, edited by N. Deruelle and T. Piran (North-Holland, Amsterdam, 1983), p. 321.
  24. J. Y. Vinet, B. J. Meers, C. N. Man, and A. Brillet, Phys. Rev. D 38, 433 (1988).
  25. B. J. Meers, Phys. Rev. D 38, 2317 (1988).
  26. S. J. Waldman et al., Classical Quantum Gravity 23, S653 (2006).
  27. F. Acernese et al., Classical Quantum Gravity 23, S635 (2006).
  28. S. Hild et al., Classical Quantum Gravity 23, S643 (2006).
  29. M. Ando et al., Phys. Rev. Lett. 86, 3950 (2001).
  30. Y. Chen and S. Kawamura, Phys. Rev. Lett. 96, 231102 (2006).
  31. F. B. Estabrook and H. D. Wahlquist, Gen. Relativ. Gravit. 6, 439 (1975).
  32. R. Schilling, Classical Quantum Gravity 14, 1513 (1997).

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Phys. Rev. D 77, 022002– Published 28 January, 2008
  • Received 11 October 2007

© 2008 American Physical Society

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