Stochastic amplitude fluctuations of bosonic dark matter and revised constraints on linear couplings. (arXiv:1905.13650v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Centers_G/0/1/0/all/0/1">Gary P. Centers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanchard_J/0/1/0/all/0/1">John W. Blanchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conrad_J/0/1/0/all/0/1">Jan Conrad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Figueroa_N/0/1/0/all/0/1">Nataniel L. Figueroa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcon_A/0/1/0/all/0/1">Antoine Garcon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gramolin_A/0/1/0/all/0/1">Alexander V. Gramolin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimball_D/0/1/0/all/0/1">Derek F. Jackson Kimball</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lawson_M/0/1/0/all/0/1">Matthew Lawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pelssers_B/0/1/0/all/0/1">Bart Pelssers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smiga_J/0/1/0/all/0/1">Joeseph A. Smiga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stadnik_Y/0/1/0/all/0/1">Yevgeny Stadnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sushkov_A/0/1/0/all/0/1">Alexander O. Sushkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wickenbrock_A/0/1/0/all/0/1">Arne Wickenbrock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budker_D/0/1/0/all/0/1">Dmitry Budker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Derevianko_A/0/1/0/all/0/1">Andrei Derevianko</a>
If the dark matter is composed of virialized particles with mass $lesssim
10$ eV, it is well described as a classical bosonic field. This field is
stochastic in nature, where the field oscillation amplitude fluctuates
following a Rayleigh distribution. Most experimental searches have been in the
regime $gtrsimmu$eV, where it is reasonable to assume a fixed field
oscillation amplitude determined by the average local dark matter energy
density. However, several direct-detection experiments are searching in the
ultra-light mass regime where the dark matter field coherence time greatly
exceeds the measurement time and the field oscillation amplitude is uncertain.
We show that the corresponding laboratory constraints of bosonic dark matter
field couplings to standard model particles are overestimated by as much as an
order of magnitude.
If the dark matter is composed of virialized particles with mass $lesssim
10$ eV, it is well described as a classical bosonic field. This field is
stochastic in nature, where the field oscillation amplitude fluctuates
following a Rayleigh distribution. Most experimental searches have been in the
regime $gtrsimmu$eV, where it is reasonable to assume a fixed field
oscillation amplitude determined by the average local dark matter energy
density. However, several direct-detection experiments are searching in the
ultra-light mass regime where the dark matter field coherence time greatly
exceeds the measurement time and the field oscillation amplitude is uncertain.
We show that the corresponding laboratory constraints of bosonic dark matter
field couplings to standard model particles are overestimated by as much as an
order of magnitude.
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