Probing dark photons with plasma haloscopes

Gelmini, Graciela B.; Millar, Alexander J.; Takhistov, Volodymyr; Vitagliano, Edoardo

doi:10.48550/arxiv.2006.06836

Cited by 3 publications

(4 citation statements)

References 91 publications

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“…Later, we had proposed a systematic approach to the astrophysical quantities in play in the empirical determination of the DM distribution [15] (hereafter Paper I). In Paper I, we also presented a likelihood function that can be used in the particle interpretation of data coming from direct and indirect searches in order to self-consistently include astrophysical uncertainties that affect our determination of the DM distribution [16][17][18][19][20][21][22][23][24].…”

Section: Introductionmentioning

confidence: 99%

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Benito

Cuoco

Iocco

2019

J. Cosmol. Astropart. Phys.

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In this work we characterize the distribution of Dark Matter (DM) in the Milky Way (MW), and its uncertainties, adopting the well known "Rotation Curve" method. We perform a full marginalization over the uncertainties of the Galactic Parameters and over the lack of knowledge on the morphology of the baryonic components of the Galaxy. The local DM density ρ 0 is constrained to the range 0.3−0.8 GeV/cm 3 at the 2σ level, and has a strong positive correlation to R 0 , the local distance from the Galactic Center. The not well-known value of R 0 is thus, at the moment, a major limitation in determining ρ 0 . Similarly, we find that the inner slope of the DM profile, γ, is very weakly constrained, showing no preference for a cored profile (γ 0) or a cuspy one (γ [1.0, 1.4]). Some combination of parameters can be, however, strongly constrained. For example the often used standard ρ 0 = 0.3 GeV/cm 3 , R 0 = 8.5 kpc is excluded at more than 4 σ. We release the full likelihood of our analysis in a tabular form over a multidimensional grid in the parameters characterizing the DM distribution, namely the scale radius R s , the scale density ρ s , the inner slope of the profile γ, and R 0 . The likelihood can be used to include the effect of the DM distribution uncertainty on the results of searches for an indirect DM signal in gamma-rays or neutrinos, from the Galactic Center (GC), or the Halo region surrounding it. As one example, we study the case of the GC excess in gamma rays. Further applications of our tabulated uncertainties in the DM distribution involve local DM searches, like direct detection and anti-matter observations, or global fits combining local and GC searches.

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Section: Introductionmentioning

confidence: 99%

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Benito

Cuoco

Iocco

2019

J. Cosmol. Astropart. Phys.

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“…A favored candidate may be the dark photon since it kinetically mixes with real photons without the need for electric or magnetic fields, and, in addition, this conversion could be resonantly enhanced if the plasma density matches the rest mass of the dark photon (A ), hω p = m A [16]. The interaction of a dark photon with a plasma medium is described, for example, in [16][17][18]. The ionospheric plasma density changes steadily, reaching a wide maximum in electron density at an altitude of about 300 km.…”

Section: The Conceptmentioning

confidence: 99%

“…The radiation flux and power of real photons due to dark photon-to-photon conversion depend on kinetic mixing, gravitational focusing, resonance effects, ionization profile, and local dark matter density (see [16,20]).…”

Section: The Conceptmentioning

confidence: 99%

Dark Matter Detection in the Stratosphere

et al. 2023

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We investigate the prospects for the direct detection of dark matter (DM) particles, incident on the upper atmosphere. A recent work relating the burst-like temperature excursions in the stratosphere at heights of ≈38–47 km with low speed incident invisible streaming matter is the motivation behind this proposal. As an example, dark photons could match the reasoning presented in that work provided they constitute part of the local DM density. Dark photons emerge as a U(1) symmetry within extensions of the standard model. Dark photons mix with real photons with the same total energy without the need for an external field, as would be required, for instance, for axions. Furthermore, the ionospheric plasma column above the stratosphere can resonantly enhance the dark photon-to-photon conversion. Noticeably, the stratosphere is easily accessible with balloon flights. Balloon missions with up to a few tons of payload can be readily assembled to operate for months at such atmospheric heights. This proposal is not limited to streaming dark photons, as other DM constituents could be involved in the observed seasonal heating of the upper stratosphere. Therefore, we advocate a combination of different types of measurements within a multi-purpose parallel detector system, in order to increase the direct detection potential for invisible streaming constituents that affect, annually and around January, the upper stratosphere.

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“…This is a common technique of searching for dark photons independent of the local dark photon abundance [18]. The latter is a less common method of dark photon detection, but was performed with a superconducting qubit [19] and has been proposed in other experiments with the benefit that they do not require a magnet [20][21][22][23]. Because the dark photon mass range is so large, there is plenty of room for these experiments to make valuable exclusions.…”

Section: Introductionmentioning

confidence: 99%

Searching for Dark Photons with Existing Haloscope Data

Ghosh,

Ruddy,

Jewell

et al. 2021

Preprint

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The dark (or hidden) photon is a massive U(1) gauge boson theorized as a dark force mediator. Dark photons can be detected with axion cavity haloscopes by probing for a power excess caused by the dark photon's kinetic mixing with Standard Model photons. Haloscope axion exclusion limits may therefore be converted into competitive dark photon parameter limits via the calculation of a corresponding dark photon to photon coupling factor. This calculation allows for an improvement in sensitivity of around four orders of magnitude relative to other dark photon exclusions and may be attained using existing data. We present how one converts haloscope axion search limits and a summary of relevant experimental parameter from published searches. Finally, we present limits on the kinetic mixing coefficient between dark photons and the Standard Model photons based on existing haloscope axion searches.

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Probing dark photons with plasma haloscopes

Cited by 3 publications

References 91 publications

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Dark Matter Detection in the Stratosphere

Searching for Dark Photons with Existing Haloscope Data

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