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Ferguson, K. R.; Anderson, A. J.; Whitehorn, N.; Ade, P. A. R.; Archipley, M.; Avva, J. S.; Balkenhol, L.; Benabed, K.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bleem, L. E.; Bouchet, F. R.; Bryant, L.; Camphuis, E.; Carlstrom, J. E.; Cecil, T. W.; Chang, C. L.; Chaubal, P.; Chichura, P. M.; Chou, T.-L.; Crawford, T. M.; Cukierman, A.; Daley, C.; de Haan, T.; Dibert, K. R.; Dobbs, M. A.; Doussot, A.; Dutcher, D.; Everett, W.; Feng, C.; Foster, A.; Galli, S.; Gambrel, A. E.; Gardner, R. W.; Goeckner-Wald, N.; Gualtieri, R.; Guidi, F.; Guns, S.; Halverson, N. W.; Hivon, E.; Holder, G. P.; Holzapfel, W. L.; Hood, J. C.; Huang, N.; Knox, L.; Korman, M.; Kuo, C.-L.; Lee, A. T.; Lowitz, A. E.; Lu, C.; Millea, M.; Montgomery, J.; Natoli, T.; Noble, G. I.; Novosad, V.; Omori, Y.; Padin, S.; Pan, Z.; Paschos, P.; Prabhu, K.; Quan, W.; Rahlin, A.; Reichardt, C. L.; Rouble, M.; Ruhl, J. E.; Schiappucci, E.; Smecher, G.; Sobrin, J. A.; Stephen, J.; Suzuki, A.; Tandoi, C.; Thompson, K. L.; Thorne, B.; Tucker, C.; Umilta, C.; Vieira, J. D.; Wang, G.; Wu, W. L. K.; Yefremenko, V.; Young, M. R.
Physical review. D, 08/2022, Letnik: 106, Številka: 4Journal Article
Ultralight axionlike particles (ALPs) are compelling dark matter candidates because of their potential to resolve small-scale discrepancies between Λ 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 gφγ 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 ( 4.7×10-22 eV≤mφ≤4.7×10-20 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 0.3 GeV/cm3 , this corresponds to gφγ<1.18×10-12 GeV-1× ( mφ1.0 × 10 - 21 eV ) . These new limits represent an improvement over the previous strongest limits set using the same effect by a factor of ~3.8 .
