Stochastic properties of ultralight scalar field gradients

Lisanti, Mariangela; Moschella, Matthew; Terrano, W. A.

doi:10.1103/physrevd.104.055037

Cited by 37 publications

(21 citation statements)

References 63 publications

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“…The properties of the UBDM field will be derived using the framework used in Refs. [31][32][33][34][35][36][37][38][39]. In brief, assuming that UBDM does not interact with itself, each individual particle can be treated as an independent classical wave.…”

Section: Stochastic Properties Of the Ultralight Bosonic Dark Matter ...mentioning

confidence: 99%

“…However, if a search is based on the measurement of the intensity of the UBDM, part of the signal is down-converted to near-zero frequency, regardless of the particular Compton frequency of the UBDM. Furthermore, assuming the standard halo model, there are stochastic fluctuations of this near-dc component [31][32][33][34][35][36][37][38][39]. The linewidth of this spectral near-dc feature is ≈ 10 6 times smaller than ω c , allowing sensors with limited bandwidth to be sensitive to UBDM with masses a million times larger than if the sensors were used to search for direct field-oscillations at ω c (as in existing and planned experiments reviewed in, for example, Refs.…”

Section: Introductionmentioning

confidence: 99%

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Intensity interferometry for ultralight bosonic dark matter detection

Masia‐Roig¹,

Figueroa²,

Ariday³

et al. 2022

Preprint

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Ultralight bosonic dark matter (UBDM) can be described by a classical wave-like field oscillating at the Compton frequency of the bosons. If a measurement scheme for the direct detection of UBDM interactions is sensitive to a signature quadratic in the field, then there is a near-zero-frequency (dc) component of the signal. Thus, a detector with a given finite bandwidth can be used to search for bosons with Compton frequencies many orders of magnitude larger than its bandwidth. This opens the possibility of a detection scheme analogous to Hanbury Brown and Twiss interferometry. Assuming that the UBDM is virialized in the gravitational potential, for example of the Milky Way, the random velocities produce slight deviations from the Compton frequency. These result in stochastic fluctuations of the intensity on a time scale determined by the spread in velocities. In order to mitigate ubiquitous local low-frequency noise, a network of sensors can be used to search for the stochastic intensity fluctuations by measuring cross-correlation between the sensors. This method is inherently broadband, since a large range of Compton frequencies will have a nearzero-frequency component within the sensor bandwidth that can be searched for simultaneously. Experiments with existing clock and magnetometer networks have sufficient sensitivity to search a broad range of unexplored parameter space.

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Section: Stochastic Properties Of the Ultralight Bosonic Dark Matter ...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Intensity interferometry for ultralight bosonic dark matter detection

Masia‐Roig¹,

Figueroa²,

Ariday³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…In the standard scenario where UDM constitutes a galactic halo [44], with ρ ⊕ DM ≡ ρ G DM 0.3 GeV/cm 3 and β ⊕ c 220 km/s, it is reasonable to assume that during the UDM virialization process around the galaxy, different patches or quasiparticles obtain random phases. This results in the UDM field-amplitude admitting stochastic fluctuations around its commonly assumed value [45][46][47][48]. In addition, we shall consider a scenario where the UDM forms a solar halo [43] with ρ ⊕ DM = 10 5 ρ G DM and β ⊕ c = 20 km/s and as long as m φ 10 −13 eV the number of patches in the halo is large and we still assume that the field amplitude is stochastic.…”

Section: Theoretical Modelmentioning

confidence: 99%

Search for oscillations of fundamental constants using molecular spectroscopy

Oswald,

Nevsky,

Vogt

et al. 2021

Preprint

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A possible implication of an ultralight dark matter (UDM) field interacting wibeginth the Standard Model (SM) degrees of freedom is oscillations of fundamental constants. Here, we establish direct experimental bounds on the coupling of an oscillating UDM field to the up, down, and strange quarks and to the gluons, for oscillation frequencies between 10 Hz and 10 8 Hz. We employ spectroscopic experiments that take advantage of the dependence of molecular transition frequencies on the nuclear masses. Our results apply to previously unexplored frequency bands, and improve on existing bounds at frequencies > 5 MHz. We identify a sector of UDM -SM coupling space where the bounds from Equivalence Principle tests may be challenged by next-generation experiments of the present kind.

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“…Moreover, the quasi-probability distribution f W evolves 5 For experiments sensitive to the gradient, the rotation of Earth introduces an amplitude modulation of the signal, leading to sidebands in the spectrum. This also introduces additional complications in the frequency space analysis [85].…”

Section: B Semiclassical Limitmentioning

confidence: 99%

Gravitational Focusing of Wave Dark Matter

Kim,

Lenoci

2021

Preprint

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A massive astrophysical object deforms a local distribution of dark matter, resulting in a local overdensity of dark matter. This phenomenon is often referred to as gravitational focusing. In the solar system, the gravitational focusing due to the Sun induces modulations of dark matter signals on terrestrial experiments. We consider the gravitational focusing of a light bosonic dark matter with a mass of less than about 10 eV. The wave nature of such dark matter candidates leads to unique signatures both in the local overdensity and in the spectrum, both of which can be experimentally relevant. We provide a formalism that captures both the gravitational focusing and the stochasticity of wave dark matter, paying particular attention to the similarity and difference to particle dark matter. Distinctive patterns in the density contrast and spectrum are observed when the de Broglie wavelength of dark matter becomes comparable or less than the size of the system and/or when the velocity dispersion of dark matter is sufficiently small. While gravitational focusing effects generally remain at a few percent level for a relaxed halo dark matter component, they could be much larger for dark matter substructures. With a few well-motivated dark matter substructures, we investigate how each substructure responds to the gravitational potential of the Sun. The limit at which wave dark matter behaves similar to particle dark matter is also discussed.

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Stochastic properties of ultralight scalar field gradients

Cited by 37 publications

References 63 publications

Intensity interferometry for ultralight bosonic dark matter detection

Intensity interferometry for ultralight bosonic dark matter detection

Search for oscillations of fundamental constants using molecular spectroscopy

Gravitational Focusing of Wave Dark Matter

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