First Results from a Broadband Search for Dark Photon Dark Matter in the 44 to 52 μeV Range with a Coaxial Dish Antenna

Creators: Knirck, Stefan; Hoshino, Gabe; Awida, Mohamed H.; Cancelo, Gustavo I.; Di Federico, Martin; Knepper, Benjamin; Lapuente, Alex; Littmann, Mira; Miller, David W.; Mitchell, Donald V.; Rodriguez, Derrick; Ruschman, Mark K.; Sawtell, Matthew A.; Stefanazzi, Leandro; Sonnenschein, Andrew; Teafoe, Gary W.; Bowring, Daniel; Carosi, G.; Chou, Aaron; Chang, Clarence L.; Dona, Kristin; Khatiwada, Rakshya; Kurinsky, Noah A.; Liu, Jesse; Pena, Cristián; Salemi, Chiara P.; Wang, Christina W.; Yu, Jialin; BREAD Collaboration

Abstract

We present first results from a dark photon dark matter search in the mass range from 44 to $52 μ eV$ (10.7–12.5 GHz) using a room-temperature dish antenna setup called GigaBREAD. Dark photon dark matter converts to ordinary photons on a cylindrical metallic emission surface with area $0.5 m^{²}$ and is focused by a novel parabolic reflector onto a horn antenna. Signals are read out with a low-noise receiver system. A first data taking run with 24 days of data does not show evidence for dark photon dark matter in this mass range, excluding dark photon photon mixing parameters $χ ≳ {10⁻¹²}$ in this range at 90% confidence level. This surpasses existing constraints by about 2 orders of magnitude and is the most stringent bound on dark photons in this range below $49 μ eV$ .

Copyright and License

Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI.

Funding

Funded by SCOAP³.

Acknowledgement

We acknowledge Abigail Vieregg and her group for providing access to the rf shielded room. We thank Dan Zhang and the ADMX Collaboration for helpful discussions about analysis. We thank all BREAD collaborators for inspiring and helpful discussions. This work is funded by the by the Department of Energy through the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. D. W. M. and G. H. would like to thank the University of Chicago Joint Task Force Initiative for its generous support for this research. J. L. is supported by a Junior Research Fellowship at Trinity College, University of Cambridge. C. P. S. is supported by the Kavli Institute for Particle Astrophysics and Cosmology Porat Fellowship.

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PhysRevLett.132.131004.pdf

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