Asteroids for ultralight dark-photon dark-matter detection
Gravitational-wave (GW) detectors that monitor fluctuations in the separation between inertial test masses (TMs) are sensitive to new forces acting on those TMs. Ultralight dark-photon dark matter (DPDM) coupled to U(1)B or U(1)B-L charges supplies one such force that oscillates with a frequency set by the DPDM mass. GW detectors operating in different frequency bands are thus sensitive to different DPDM mass ranges. A recent GW detection proposal based on monitoring the separation of certain asteroids in the inner Solar System would have sensitivity to μHz frequencies. In this paper, we show how that proposal would also enable access to new parameter space for DPDM coupled to B[respectively, B - L] charges in the mass range 5[9] x 10-21 eV ≲ mDM ≲ 2 x 10-19 eV, with peak sensitivities about a factor of 500 [50] beyond current best limits on ϵB [ϵB-L] at mDM ~ 2 x 10-19 eV. Sensitivity could extended up to mDM ~ 2 x 10-18 eV only if noise issues associated with asteroid rotational motion could be overcome.
- Research Organization:
- Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Johns Hopkins University, Baltimore, MD (United States)
- Sponsoring Organization:
- USDOE Office of Science (SC), High Energy Physics (HEP); Simons Investigator Grant
- Grant/Contract Number:
- AC02-07CH11359; 827042
- OSTI ID:
- 1923392
- Alternate ID(s):
- OSTI ID: 1898755
- Report Number(s):
- FERMILAB-PUB-22-850-SQMS-V; arXiv:2210.09324; PRVDAQ; 043004
- Journal Information:
- Physical Review D, Journal Name: Physical Review D Vol. 107 Journal Issue: 4; ISSN 2470-0010
- Publisher:
- American Physical SocietyCopyright Statement
- Country of Publication:
- United States
- Language:
- English
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