Nonvirialized axion search sensitive to Doppler effects in the Milky Way halo
Creators
- Bartram, C.
- Braine, T.
- Cervantes, R.
-
Crisosto, N.
- Du, N.
- Goodman, C.
-
Guzzetti, M.
- Hanretty, C.
- Lee, S.
- Leum, G.
- Rosenberg, L. J
- Rybka, G.
- Sinnis, J.
- Zhang, D.
- Awida, M. H.
- Bowring, D.
- Chou, A. S.
- Hollister, M.
- Knirck, S.
- Sonnenschein, A.
- Wester, W.
- Khatiwada, R.
- Brodsky, J.
- Carosi, G.
- Duffy, L. D.
- Goryachev, M.
- McAllister, B.
- Quiskamp, A.
- Thomson, C.
- Tobar, M. E.
- Boutan, C.
- Jones, M.
- LaRoque, B. H.
- Lentz, E.
- Man, N. E.
- Oblath, N. S.
- Taubman, M. S.
- Yang, J.
- Clarke, John
- Siddiqi, I.
- Agrawal, A.
- Dixit, A. V.
- Gleason, J. R.
- Han, Y.
- Hipp, A. T.
- Jois, S.
- Sikivie, P.
- Sullivan, N. S.
- Tanner, D. B.
- Daw, E. J.
- Perry, M. G.
- Buckley, J. H.
- Gaikwad, C.
- Hoffman, J.
- Murch, K. W.
- Russell, J.
- ADMX Collaboration
Abstract
The Axion Dark Matter eXperiment (ADMX) has previously excluded Dine-Fischler-Srednicki-Zhitnisky (DFSZ) axions between 680–790 MHz under the assumption that the dark matter is described by the isothermal halo model. However, the precise nature of the velocity distribution of dark matter is still unknown, and alternative models have been proposed. We report the results of a nonvirialized axion search over the mass range 2.81–3.31 μeV, corresponding to the frequency range 680–800 MHz. This analysis marks the most sensitive search for nonvirialized axions sensitive to Doppler effects in the Milky Way Halo to date. Accounting for frequency shifts due to the detector’s motion through the Galaxy, we exclude cold flow relic axions with a velocity dispersion of 𝒪(10⁻⁷)c with 95% confidence.
Copyright and License
© 2024 American Physical Society.
Acknowledgement
This work was supported by the U.S. Department of Energy through Grants No. DE-SC0009800, No. DE-SC0009723, No. DE-SC0010296, No. DE-SC0010280, No. DE-SC0011665, No. DE-FG02-97ER41029, No. DE-FG02-96ER40956, No. DE-AC52-07NA27344, No. DE-AC03-76SF00098, No. DE-SC-0022148, and No. DE-SC0017987. This document was prepared by the ADMX Collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, Office of High Energy Physics HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. Pacific Northwest National Laboratory (PNNL) is operated by Battelle Memorial Institute for the DOE under Contract No. DE-AC05-76RL01830. UWA participation is funded by the ARC Centre of Excellence for Engineered Quantum Systems, Grant No. CE170100009, Dark Matter Particle Physics, Grant No. CE200100008, and Forrest Research Foundation. Chelsea Bartram acknowledges support from the Panofsky Fellowship at SLAC. The Sheffield group acknowledges support from the UK Science and Technology Facilities Council (STFC) under grants ST/T006811/1 and ST/X005879/1. LLNL Release Number: LLNL-JRNL-853502. LANL Release Number: LA-UR-24-21433. PNNL Release Number: PNNL-SA-195179.
Files
PhysRevD.109.083014.pdf
Additional details
Identifiers
- ISSN
- 2470-0029
Funding
- United States Department of Energy
- DE-SC0009800
- United States Department of Energy
- DE-SC0009723
- United States Department of Energy
- DE-SC0010296
- United States Department of Energy
- DE-SC0010280
- United States Department of Energy
- DE-SC0011665
- United States Department of Energy
- DE-FG02-97ER41029
- United States Department of Energy
- DE-FG02-96ER40956
- United States Department of Energy
- DE-AC52-07NA27344
- United States Department of Energy
- DE-AC03-76SF00098
- United States Department of Energy
- DE-SC-0022148
- United States Department of Energy
- DE-SC0017987
- United States Department of Energy
- DE-AC02-07CH11359
- Forrest Research Foundation
- Science and Technology Facilities Council
- ST/T006811/1
- Science and Technology Facilities Council
- ST/X005879/1
- Australian Research Council
- CE170100009
- Australian Research Council
- CE200100008
- SLAC National Accelerator Laboratory