R. Abbott

Author ORCID Identifier

Chiadini, Francesco: 0000-0002-9339-8622
Nelemans, Gijs: 0000-0002-0752-2974
Ferrante, Isidoro: 0000-0002-0083-7228
Helmling-Cornell, Adrian: 0000-0002-7709-8638
Ando, Masaki: 0000-0002-8865-9998
Shcheblanov, Nikita: 0000-0001-8696-2435
Mow-Lowry, Conor M: 0000-0002-0351-4555
Christensen, Nelson: 0000-0002-6870-4202
Hollows, Ian: 0000-0002-3404-6459
Kakizaki, Mitsuru: 0000-0003-1430-3339
Pan, Kuo-Chuan: 0000-0002-1473-9880
Shao, Lijing: 0000-0002-1334-8853
Keitel, David: 0000-0002-2824-626X
Mitselmakher, Guenakh: 0000-0001-5745-3658
Gibson, Desmond: 0000-0003-2851-0072
Zhao, Gongbo: 0000-0003-4726-6714
Edelman, Bruce: 0000-0001-7648-1689
Edy, Oliver: 0000-0001-9617-8724
Singh, Neha: 0000-0002-1135-3456
Sordini, Viola: 0000-0003-0885-824X
Harry, Ian: 0000-0002-5304-9372
Nuttall, Laura Kate: 0000-0001-7472-0201
Macas, Ronaldas: 0000-0002-6096-8297
Allocca, Annalisa: 0000-0002-5288-1351
Williamson, Andrew: 0000-0002-7627-8688
Garcia Nunez, Carlos: 0000-0001-5518-6189
Steer, Daniele: 0000-0002-8781-1273
Mozzon, Simone: 0000-0002-8855-2509
Di Renzo, Francesco: 0000-0002-5447-3810
Nakano, Hiroyuki: 0000-0001-7665-0796
Parisi, Alessandro: 0000-0003-0251-8914
Park, June Gyu: 0000-0002-7510-0079
Lundgren, Andrew: 0000-0002-0363-4469
Razzano, Massimiliano: 0000-0003-4825-1629
Perries, Stephane: 0000-0003-2213-3579

Document Type


Publication Date



We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo's third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between m(A) similar to 10(-14)-10(-11) eV/c(2), which corresponds to frequencies between 10-2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e., U(1)(B) dark matter. For the cross-correlation method, the best median constraint on the squared coupling is similar to 1.31 x 10(-47) at m(A) similar to 4.2 x 10(-13) eV/c(2); for the other analysis, the best constraint is similar to 2.4 x 10(-47) at m(A) similar to 5.7 x 10(-13) eV/c(2). These limits improve upon those obtained in direct dark matter detection experiments by a factor of similar to 100 for m(A) similar to [2-4] x 10(-13) eV/c(2), and are, in absolute terms, the most stringent constraint so far in a large mass range m(A) similar to 2 x 10(-13) - 8 x 10(-12) eV/c(2).

Publication Source (Journal or Book title)

Physical Review D