Symmetries and selection rules: optimising axion haloscopes for Gravitational Wave searches

Domcke, Valerie; Garcia-Cely, Camilo; Lee, Sung Mook; Rodd, Nicholas L.

doi:10.1007/jhep03(2024)128

Cited by 9 publications

(2 citation statements)

References 56 publications

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“…This resembles the coupling between gravity and the EM sector via the term L ⊃ hF 2 . The similarity implies that both axions and gravitons can convert to photons in external magnetic fields and that data from existing axion haloscopes can be reinterpreted to constrain HFGWs [58,59]. In general, approach (ii) has the advantage of having full knowledge and control of the magnetic field.…”

Section: Alternative Methods To Probe Hfgwmentioning

confidence: 99%

“…(ii) Laboratory settings: although experiments specifically dedicated to inverse Gertsenshtein effect are yet to be conducted, existing instruments that involve controlled magnetic fields and electromagnetic (EM) sensors, such as axion detectors, can be repurposed and their results reinterpreted as upper limits on HFGWs [53][54][55][56][57][58][59][60][61][62][63].…”

Section: Jcap05(2024)051mentioning

confidence: 99%

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Inverse Gertsenshtein effect as a probe of high-frequency gravitational waves

He,

Giri,

Sharma

et al. 2024

J. Cosmol. Astropart. Phys.

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We apply the inverse Gertsenshtein effect, i.e., the graviton-photon conversion in the presence of a magnetic field, to constrain high-frequency gravitational waves (HFGWs). Using existing astrophysical measurements, we compute upper limits on the GW energy densities ΩGW at 16 different frequency bands. Given the observed magnetisation of galaxy clusters with field strength B ∼ μG correlated on 𝒪(10) kpc scales, we estimate HFGW constraints in the 𝒪(102) GHz regime to be ΩGW ≲ 1016 with the temperature measurements of the Atacama Cosmology Telescope (ACT). Similarly, we conservatively obtain ΩGW ≲ 1013 (1011) in the 𝒪(102) MHz (𝒪(10) GHz) regime by assuming uniform magnetic field with strength B ∼ 0.1 nG and saturating the excess signal over the Cosmic Microwave Background (CMB) reported by radio telescopes such as the Experiment to Detect the Global EoR Signature (EDGES), LOw Frequency ARray (LOFAR), and Murchison Widefield Array (MWA), and the balloon-borne second generation Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE2) with graviton-induced photons. The upcoming Square Kilometer Array (SKA) can tighten these constraints by roughly 10 orders of magnitude, which will be a step closer to reaching the critical value of ΩGW = 1 or the Big Bang Nucleosynthesis (BBN) bound of ΩGW ≃ 1.2 × 10-6. We point to future improvement of the SKA forecast and estimate that proposed CMB measurement at the level of 𝒪(100-2) nK, such as Primordial Inflation Explorer (PIXIE) and Voyage 2050, are needed to viably detect stochastic backgrounds of HFGWs.

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Section: Alternative Methods To Probe Hfgwmentioning

confidence: 99%

Section: Jcap05(2024)051mentioning

confidence: 99%

Inverse Gertsenshtein effect as a probe of high-frequency gravitational waves

He,

Giri,

Sharma

et al. 2024

J. Cosmol. Astropart. Phys.

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A coordinate-independent formalism for detecting high-frequency gravitational waves

Ratzinger,

Schenk,

Schwaller

2024

J. High Energ. Phys.

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In an external electric or magnetic field, a gravitational wave (GW) may be converted into electromagnetic radiation. We present a coordinate-invariant framework to describe the GW signal in a detector that is based on this effect, such as cavities for axion searches. In this framework, we pay special attention to the definition of manifestly coordinate-independent expressions for the electromagnetic fields that an external observer would detect. A careful assessment of the detector’s perceived motion allows us to treat both its mechanical and its electromagnetic response to the GW consistently. We further introduce well-defined approximations for which this motion may be neglected, and hence provide suggestions on which coordinate frame is suitable to characterise the GW signal in practice. We illustrate our findings in two examples, an infinitesimally thin rod and a spherical electromagnetic cavity.

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Searching for high-frequency gravitational waves with phonons

Kahn,

Schütte-Engel,

Trickle

2024

Phys. Rev. D

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The gravitational wave (GW) spectrum at frequencies above a kHz is a largely unexplored frontier. We show that detectors with sensitivity to single-phonon excitations in crystal targets can search for GWs with frequencies, 1 THz≲f≲100 THz, corresponding to the range of optical phonon energies, 1 meV≲ω≲100 meV. Such detectors are already being built to search for light dark matter (DM), and therefore sensitivity to high-frequency GWs will be achieved as a byproduct. We begin by deriving the absorption rate of a general GW signal into single phonons. We then focus on carefully defining the detector sensitivity to monochromatic and chirp signals, and compute the detector sensitivity for many proposed light DM detection targets. The detector sensitivity is then compared to the signal strength of candidate high-frequency GW sources, e.g., superradiant annihilation and black hole inspiral, as well as other recent detector proposals in the 1 MHz≲f≲100 THz frequency range. With a judicious choice of target materials, a collection of detectors could optimistically achieve sensitivities to monochromatic signals with h0∼10−23−10−25 over 1 THz≲f≲100 THz. Published by the American Physical Society 2024

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Symmetries and selection rules: optimising axion haloscopes for Gravitational Wave searches

Cited by 9 publications

References 56 publications

Inverse Gertsenshtein effect as a probe of high-frequency gravitational waves

Inverse Gertsenshtein effect as a probe of high-frequency gravitational waves

A coordinate-independent formalism for detecting high-frequency gravitational waves

Searching for high-frequency gravitational waves with phonons

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