Superradiant searches for dark photons in two stage atomic transitions

Bhoonah, Amit; Bramante, Joseph; Song, Ningqiang

doi:10.1103/physrevd.101.055040

Cited by 8 publications

(7 citation statements)

References 74 publications

(111 reference statements)

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“…Although we run the risk of being overly-stringent, we adopt the most democratic approach of taking the lower envelope of all published analyses, including: Arias et al [39], Witte et al [119,120], and Caputo et al [121,122], though we note that there are some substantive disagreements between these analyses. Three astrophysical limits also require DPDM: those based on the heating of the intergalactic medium (IGM) [123], the gas in the Leo T dwarf [124], and the gas cloud at the galactic centre G357.8-4.7-55 [125], and again, there are also disagreements between these analyses.…”

Section: Dpdm Heating Dpdm Heatingmentioning

confidence: 99%

“…1 and 10 will also see improvements over the next few years. For example, upgraded LSW experiments [195][196][197], experiments using atomic transitions [125,198,199], or Aharanov-Bohm experiments [200,201] may improve the purely-laboratory bounds on DPs. Whereas searches using X-ray [202] and radio [203,204] telescopes, fast radio burst timing [205], or asteroseismology [206], may improve upon existing astrophysical bounds.…”

Section: E Optimising Future Experimentsmentioning

confidence: 99%

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Dark photon limits: a handbook

Caputo,

Millar,

O'Hare

et al. 2021

Preprint

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The dark photon is a massive hypothetical particle that interacts with the Standard Model by kinetically mixing with the visible photon. For small values of the mixing parameter, dark photons can evade cosmological bounds to be a viable dark matter candidate. Due to the similarities with the electromagnetic signals generated by axions, several bounds on dark photon signals are simply reinterpretations of historical bounds set by axion haloscopes. However, the dark photon has a property that the axion does not: an intrinsic polarisation. Due to the rotation of the Earth, accurately accounting for this polarisation is nontrivial, and highly experiment-dependent. We show that if one does account for this polarisation, and the rotation of the Earth, experimental sensitivity to the dark photon's kinetic mixing parameter can be improved by over an order of magnitude. We detail the strategies that would need to be taken to properly optimise a dark photon search. These include judiciously choosing the location and orientation of the experiment, as well as strategically timing any repeated measurements. We also point out that several well-known searches for axions employ techniques for testing signals that preclude their ability to set exclusion limits on dark photons, and hence should not be reinterpreted as such.

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Section: Dpdm Heating Dpdm Heatingmentioning

confidence: 99%

Section: E Optimising Future Experimentsmentioning

confidence: 99%

Dark photon limits: a handbook

Caputo,

Millar,

O'Hare

et al. 2021

Preprint

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“…With coupling to electron, a light mediator, such as axion [134] and dark photon [135], can also be directly produced in this coherently stimulated process, |e → |g + γ + a/γ . Experimentally, there is no distinction whether the final state is a neutrino pair, axion, or dark photon.…”

Section: Sensitivity and Physics Reachmentioning

confidence: 99%

Probing light mediators in the radiative emission of neutrino pair

Pasquini

2022

Eur. Phys. J. C

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We propose a new possibility of using the coherently enhanced neutrino pair emission to probe light-mediator interactions between electron and neutrinos. With typical momentum transfer at the atomic $$\mathcal O(1$$ O ( 1 eV) scale, this process is extremely sensitive for the mediator mass range $$\mathcal O(10^{-3} \sim 10^4$$ O ( 10 - 3 ∼ 10 4 ) eV. The sensitivity on the product of couplings with electron ($$g^e$$ g e or $$y^e$$ y e ) and neutrinos ($$g^\nu $$ g ν or $$y^\nu $$ y ν ) can touch down to $$|y^e y^\nu | < 10^{-9} \sim 10^{-19}$$ | y e y ν | < 10 - 9 ∼ 10 - 19 for a scalar mediator and $$|g^e g^\nu | < 10^{-15} \sim 10^{-26}$$ | g e g ν | < 10 - 15 ∼ 10 - 26 for a vector one, with orders of improvement from the existing constraints.

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“…(35) and (39), respectively. The brown region (DPDM) corresponds to the preexisting constraints on the dark photon DM [14,25,[96][97][98][99][100][101][102]. The current best bounds come from cooling of young neutron stars (NS+SN1987A) [86,103], from cooling of the Sun, horizontal branch stars, and red giants (Sun+HB+RG) [87,88], from transitions of SM photons to dark photons (γ → γ ) [100,[104][105][106][107][108][109], and from blackhole superradiance (BHSR) [74][75][76].…”

Section: Constraintsmentioning

confidence: 99%

Particle dispersion in the classical vector dark matter background

Chun¹,

Yun²

2022

Preprint

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Interactions with a background medium modify in general the dispersion relation and canonical normalization of propagating particles. This can have an important phenomenological consequence when considering light dark matter coupling to quarks and leptons. In this paper, we address this issue in the vector dark matter background with the randomly distributed polarizations or a fixed polarization to the single direction. The observations associated with particle dispersion can give constraints on new light Abelian gauge boson models. Considering the solar neutrino transition and the electron mass measurement, stringent bounds can be put on the gauged Lµ − Lτ model and the dark photon model. Moreover, the classical vector field turns out to induce drastic changes in the particle normalization, which rule out a significant parameter region of the generic vector dark matter model.

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Superradiant searches for dark photons in two stage atomic transitions

Cited by 8 publications

References 74 publications

Dark photon limits: a handbook

Dark photon limits: a handbook

Probing light mediators in the radiative emission of neutrino pair

Particle dispersion in the classical vector dark matter background

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