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Pulsar timing signal from ultralight scalar dark matter · Around

2013

Pulsar timing signal from ultralight scalar dark matter

Khmelnitsky, Andrei, Rubakov, Valery

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An ultralight free scalar field with mass around 10^{-23} - 10^{-22} eV is a viable dark mater candidate, which can help to resolve some of the issues of the cold dark matter on sub-galactic scales.

We consider the gravitational field of the galactic halo composed out of such dark matter.
The scalar field has oscillating in time pressure, which induces oscillations of gravitational potential with amplitude of the order of 10^{-15} and frequency in the nanohertz range.
This frequency is in the range of pulsar timing array observations.

Built on

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L. Amendola and R. Barbieri, “Dark matter from an ultra-light pseudo-Goldsone-boson,” Phys. Lett. B 642
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Similar

F. A. Jenet, G. B. Hobbs, W. van Straten, R. N. Manchester, M. Bailes, J. P. W. Verbiest, R. T. Edwards and A. W. Hotan et al
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M. Kramer, 2, D. C. Backer, J. M. Cordes, T. J. W. Lazio, B. W. Stappers and S. Johnston, “Strong-field tests of gravity using pulsars and black holes,” New Astron. Rev. 48
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2009
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A. Sesana, A. Vecchio and C. N. Colacino, “The stochastic gravitational-wave background from massive black hole binary systems: implications for observations with Pulsar Timing Arrays,” arXiv:0804.4476 [astro-ph]; A. Sesana and A. Vecchio, “Gravitational waves and pulsar timing: stochastic background, individual sources and parameter estimation,” Class. Quant. Grav. 27
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G. Hobbs, F. Jenet, K. J. Lee, J. P. W. Verbiest, D. Yardley, R. Manchester, A. Lommen and W. Coles et al
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Then

D. J. E. Marsh and P. G. Ferreira, “Ultra-Light Scalar Fields and the Growth of Structure in the Universe,” Phys. Rev. D 82
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Later among the works it cites.
Z. L. Wen, F. A. Jenet, D. Yardley, G. B. Hobbs and R. N. Manchester, “Constraining the coalescence rate of supermassive black-hole binaries using pulsar timing,” Astrophys. J. 730
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2011
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J. Magana and T. Matos, “A brief Review of the Scalar Field Dark Matter model,” J. Phys. Conf. Ser. 378
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