Kavli Affiliate: Chao-Lin Kuo
| First 5 Authors: K. R. Ferguson, A. J. Anderson, N. Whitehorn, P. A. R. Ade, M. Archipley
| Summary:
Ultralight axionlike particles (ALPs) are compelling dark matter candidates
because of their potential to resolve small-scale discrepancies between
$Lambda$CDM predictions and cosmological observations. Axion-photon coupling
induces a polarization rotation in linearly polarized photons traveling through
an ALP field; thus, as the local ALP dark matter field oscillates in time,
distant static polarized sources will appear to oscillate with a frequency
proportional to the ALP mass. We use observations of the cosmic microwave
background from SPT-3G, the current receiver on the South Pole Telescope, to
set upper limits on the value of the axion-photon coupling constant
$g_{phigamma}$ over the approximate mass range $10^{-22} – 10^{-19}$ eV,
corresponding to oscillation periods from 12 hours to 100 days. For periods
between 1 and 100 days ($4.7 times 10^{-22} text{ eV} leq m_phi leq 4.7
times 10^{-20} text{ eV}$), where the limit is approximately constant, we set
a median 95% C.L. upper limit on the amplitude of on-sky polarization rotation
of 0.071 deg. Assuming that dark matter comprises a single ALP species with a
local dark matter density of $0.3text{ GeV/cm}^3$, this corresponds to
$g_{phigamma} < 1.18 times 10^{-12}text{ GeV}^{-1} times left(
frac{m_{phi}}{1.0 times 10^{-21} text{ eV}} right)$. These new limits
represent an improvement over the previous strongest limits set using the same
effect by a factor of ~3.8.
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