APS : Search for a Dark-Matter-Induced Cosmic Axion Background with ADMX

Nitta, T.; Chou, A.S.; Murayama, H.; Quiskamp, A.; Gaikwad, C.; Bartram, C.; Goryachev, M.; Hollister, M.; Siddiqi, I.; Tanner, D.B.; Taubman, M.S.; Rosenberg, L.J.; Sikivie, P.; Thomson, C.; Sullivan, N.S.; Sinnis, J.; Boutan, C.; Khatiwada, R.; Leum, G.; Oblath, N.S.; Perry, M.G.; Buckley, J.H.; Lentz, E.; Awida, M.H.; Knirck, S.; Hanretty, C.; Tobar, M.E.; Braine, T.; Hartman, E.; Rybka, G.; Yang, J.; Gleason, J.R.; Duffy, L.D.; Du, N.; Hipp, A.T.; Hoffman, J.; Murch, K.W.; Sonnenschein, A.; Rodd, N.L.; Daw, E.J.; Carosi, G.; Wester, W.; McAllister, B.T.; Guzzetti, M.; Clarke, John; Dror, J.A.; Robertson, N.

doi:10.1103/PhysRevLett.131.101002

Article
Report number	arXiv:2303.06282 ; FERMILAB-PUB-23-109-PPD-SQMS
Title	Search for a Dark-Matter-Induced Cosmic Axion Background with ADMX
Related title	Search for the Cosmic Axion Background with ADMX
Author(s)	Nitta, T. (Washington U., Seattle) ; Braine, T. (Washington U., Seattle) ; Du, N. (Washington U., Seattle) ; Guzzetti, M. (Washington U., Seattle) ; Hanretty, C. (Washington U., Seattle) ; Leum, G. (Washington U., Seattle) ; Rosenberg, L.J. (Washington U., Seattle) ; Rybka, G. (Washington U., Seattle) ; Sinnis, J. (Washington U., Seattle) ; Clarke, John (UC, Berkeley) ; Siddiqi, I. (UC, Berkeley) ; Awida, M.H. (Fermilab) ; Chou, A.S. (Fermilab) ; Hollister, M. (Fermilab) ; Knirck, S. (Fermilab) ; Sonnenschein, A. (Fermilab) ; Wester, W. (Fermilab) ; Gleason, J.R. (Florida U.) ; Hipp, A.T. (Florida U.) ; Sikivie, P. (Florida U.) ; Sullivan, N.S. (Florida U.) ; Tanner, D.B. (Florida U.) ; Khatiwada, R. (IIT, Chicago ; Fermilab) ; Carosi, G. (LLNL, Livermore) ; Robertson, N. (LLNL, Livermore) ; Duffy, L.D. (Los Alamos) ; Boutan, C. (PNL, Richland) ; Lentz, E. (PNL, Richland) ; Oblath, N.S. (PNL, Richland) ; Taubman, M.S. (PNL, Richland) ; Yang, J. (PNL, Richland) ; Daw, E.J. (Sheffield U.) ; Perry, M.G. (Sheffield U.) ; Bartram, C. (SLAC) ; Buckley, J.H. (Washington U., St. Louis) ; Gaikwad, C. (Washington U., St. Louis) ; Hoffman, J. (Washington U., St. Louis) ; Murch, K.W. (Washington U., St. Louis) ; Goryachev, M. (Western Australia U.) ; Hartman, E. (Western Australia U.) ; McAllister, B.T. (Western Australia U. ; Swinburne U. Tech., Hawthorn) ; Quiskamp, A. (Western Australia U.) ; Thomson, C. (Western Australia U.) ; Tobar, M.E. (Western Australia U.) ; Dror, J.A. (UC, Santa Cruz, Inst. Part. Phys.) ; Murayama, H. (UC, Berkeley) ; Rodd, N.L. (CERN)
Publication	2023-09-08
Imprint	2023-03-10
Number of pages	7
In:	Phys. Rev. Lett. 131 (2023) 101002
DOI	10.1103/PhysRevLett.131.101002 (publication)
Subject category	hep-ex ; Particle Physics - Experiment
Accelerator/Facility, Experiment	ADMX
Abstract	We report the first result of a direct search for a Cosmic ${\it axion}$ Background (C$a$B) - a relativistic background of axions that is not dark matter - performed with the axion haloscope, the Axion Dark Matter eXperiment (ADMX). Conventional haloscope analyses search for a signal with a narrow bandwidth, as predicted for dark matter, whereas the C$a$B will be broad. We introduce a novel analysis strategy, which searches for a C$a$B induced daily modulation in the power measured by the haloscope. Using this, we repurpose data collected to search for dark matter to set a limit on the axion photon coupling of a C$a$B originating from dark matter cascade decay via a mediator in the 800-995 MHz frequency range. We find that the present sensitivity is limited by fluctuations in the cavity readout as the instrument scans across dark matter masses. Nevertheless, we suggest that these challenges can be surmounted using superconducting qubits as single photon counters, and allow ADMX to operate as a telescope searching for axions emerging from the decay of dark matter. The daily modulation analysis technique we introduce can be deployed for various broadband RF signals, such as other forms of a C$a$B or even high-frequency gravitational waves.
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0) publication: © 2023-2025 authors (License: CC BY 4.0), sponsored by SCOAP³

${\it Left:} a schematic depiction of the spatial coherence of a dark matter (orange) or \CaB (light blue) signal over the ${\rm TM}_{010}$ mode of a cylindrical cavity. The dark matter signal is coherent across the cavity, and therefore independent of the incident direction, whereas the \CaB is not, and therefore the dashed and solid curves can give rise to significantly different signals. {\it Right:} a quantification of this effect using the expression in Eq.~\eqref{eq:K}, where $\alpha$ is the angle between the incident axion and the cavity magnetic field, $R=0.2$~m, and $L=1$~m. The power of photons converted from the \CaB is maximized at $\alpha=\pi/2$, when the cavity magnetic field is perpendicular to the incident axions, and suppressed when $\alpha=0$.$ ${\it Left:} a schematic depiction of the spatial coherent length of a dark matter ($\lambda_{\rm DM}\sim {\cal O}(100~{\rm m})$, orange) or \CaB ($\lambda_{\CaB}\sim {\cal O}(0.1~{\rm m})$, light blue) signal over the ${\rm TM}_{010}$ mode of a cylindrical cavity ($d_{\rm cav}\sim {\cal O}(0.1~{\rm m})$, black cylinder). The dark matter signal is coherent across the cavity, and therefore independent of the incident direction, whereas the \CaB is not, and therefore the dashed and solid curves can give rise to significantly different signals. {\it Right:} a quantification of this effect using the expression in Eq.~\eqref{eq:K}, where $\alpha$ is the angle between the incident axion and the cavity magnetic field, $R=0.2$~m, and $L=1$~m. The power of photons converted from the \CaB is maximized at $\alpha=\pi/2$, when the cavity magnetic field is perpendicular to the incident axions, and suppressed when $\alpha=0$.$ ${\it Top:} an example of the mean power (gray) as a function of time collected on April 30, 2021. We further show the JPA gain in green, and in the inset demonstrate the two are strongly correlated. {\it Bottom:} For the same dataset, we divide the mean power out by the gain (left axis) and show the results PEM computed according to Eq.~\eqref{eq:powerexess} (right axis).$ Show more plots

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Record created 2023-03-15, last modified 2024-12-20

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