Axion Dark Matter Search with Interferometric Gravitational Wave Detectors. (arXiv:1903.02017v1 [hep-ph])

Axion Dark Matter Search with Interferometric Gravitational Wave Detectors. (arXiv:1903.02017v1 [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:+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>, <a href="http://arxiv.org/find/hep-ph/1/au:+Obata_I/0/1/0/all/0/1">Ippei Obata</a>

Axion dark matter differentiates the phase velocities of the
circular-polarized photons. In this Letter, a scheme to measure the phase
difference by using a linear optical cavity is proposed. 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 $g_{text{a}gamma} simeq
8times10^{-13}$ GeV$^{-1}, (4 times 10^{-14}$ 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 $g_{text{a}gamma} simeq 10^{-14}$
GeV$^{-1}$ $(8times10^{-17}$ 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 this Letter, a scheme to measure the phase
difference by using a linear optical cavity is proposed. 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 $g_{text{a}gamma} simeq
8times10^{-13}$ GeV$^{-1}, (4 times 10^{-14}$ 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 $g_{text{a}gamma} simeq 10^{-14}$
GeV$^{-1}$ $(8times10^{-17}$ 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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