Axion Dark Matter Search with Interferometric Gravitational Wave Detectors. (arXiv:1912.09123v1 [hep-ph])

Axion Dark Matter Search with Interferometric Gravitational Wave Detectors. (arXiv:1912.09123v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Nagano_K/0/1/0/all/0/1">Koji Nagano</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Obata_I/0/1/0/all/0/1">Ippei Obata</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Fujita_T/0/1/0/all/0/1">Tomohiro Fujita</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Michimura_Y/0/1/0/all/0/1">Yuta Michimura</a>

Axion dark matter differentiates the phase velocities of the
circular-polarized photons. In Phys.Rev.Lett. 123 (2019) no.11, 111301, we have
proposed a scheme to measure the phase difference by using a linear optical
cavity. If the scheme is applied to the Fabry-P’erot arm of Advanced LIGO-like
(Cosmic-Explorer-like) gravitational wave detector, the potential sensitivity
to the axion-photon coupling constant, $g_{text{a}gamma}$, reaches
$g_{text{a}gamma} simeq 8times10^{-13} text{GeV}^{-1}, (4 times
10^{-14}text{GeV}^{-1})$ at the axion mass $m simeq 3times 10^{-13}$ eV
($2times10^{-15}$ eV) and remains at around this sensitivity for 3 orders of
magnitude in mass. Furthermore, its sensitivity has a sharp peak reaching
$g_{text{a}gamma} simeq 10^{-14} text{GeV}^{-1} (8times10^{-17}
text{GeV}^{-1})$ at $m = 1.563times10^{-10}$ eV ($1.563times10^{-11}$ eV).
This sensitivity can be achieved without loosing any sensitivity to
gravitational waves.

Axion dark matter differentiates the phase velocities of the
circular-polarized photons. In Phys.Rev.Lett. 123 (2019) no.11, 111301, we have
proposed a scheme to measure the phase difference by using a linear optical
cavity. If the scheme is applied to the Fabry-P’erot arm of Advanced LIGO-like
(Cosmic-Explorer-like) gravitational wave detector, the potential sensitivity
to the axion-photon coupling constant, $g_{text{a}gamma}$, reaches
$g_{text{a}gamma} simeq 8times10^{-13} text{GeV}^{-1}, (4 times
10^{-14}text{GeV}^{-1})$ at the axion mass $m simeq 3times 10^{-13}$ eV
($2times10^{-15}$ eV) and remains at around this sensitivity for 3 orders of
magnitude in mass. Furthermore, its sensitivity has a sharp peak reaching
$g_{text{a}gamma} simeq 10^{-14} text{GeV}^{-1} (8times10^{-17}
text{GeV}^{-1})$ at $m = 1.563times10^{-10}$ eV ($1.563times10^{-11}$ eV).
This sensitivity can be achieved without loosing any sensitivity to
gravitational waves.

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