New results from HAYSTAC’s phase II operation with a squeezed state receiver

Jewell, M. J.; Leder, A.; Backes, Kelly; Bai, Xiran; Bibber, K. van; Brubaker, Benjamin; Cahn, S. B.; Droster, Alex; Esmat, Maryam H.; Ghosh, Sumita; Graham, Eleanor A. M.; Hilton, G. C.; Jackson, H. J.; Laffan, Claire; Lamoreaux, S. K.; Lehnert, K. W.; Lewis, Samantha M.; Malnou, M.; Maruyama, R.; Palken, Daniel; Rapidis, N. M.; Ruddy, E. P.; Simanovskaia, Maria; Singh, Sukhman; Speller, D.; Vale, Leila R.; Wang, H.; Zhu, Yuqi

doi:10.1103/physrevd.107.072007

Cited by 23 publications

(7 citation statements)

References 59 publications

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“…The green-shaded region shows the collective constraint (as compiled in ref. [39]) from various haloscope experiments: ADMX [43], HAYSTAC [156,157], ORGAN [158], UPLOAD [159], RBF [160,161], UF [162], CAPP [163][164][165][166][167], CAST-CAPP [168], QUAX [169,170], BASE [171], and TASEH [172]. The yellow-shaded region is the astrophysical constraint from the R 2 parameter [47] (top right, just below CAST) and from pulsar data [50].…”

Section: Galactic Center Versus Anti-centermentioning

confidence: 99%

On the Galactic radio signal from stimulated decay of axion dark matter

Bhupal Dev,

Ferrer,

Okawa

2024

J. Cosmol. Astropart. Phys.

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We study the full-sky distribution of the radio emission from the stimulated decay of axions which are assumed to compose the dark matter in the Galaxy. Besides the constant extragalactic and CMB components, the decays are stimulated by a Galactic radio emission with a spatial distribution that we empirically determine from observations. We compare the diffuse emission to the counterimages of the brightest supernovæ remnants, and take into account the effects of free-free absorption. We show that, if the dark matter halo is described by a cuspy NFW profile, the expected signal from the Galactic center is the strongest. Interestingly, the emission from the Galactic anti-center provides competitive constraints that do not depend on assumptions on the uncertain dark matter density in the inner region. Furthermore, the anti-center of the Galaxy is the brightest spot if the Galactic dark matter density follows a cored profile. The expected signal from stimulated decays of axions of mass ma ∼ 10-6 eV is within reach of the Square Kilometer Array for an axion-photon coupling gaγ ≳ (2-3) × 10-11 GeV-1.

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Section: Galactic Center Versus Anti-centermentioning

confidence: 99%

On the Galactic radio signal from stimulated decay of axion dark matter

Bhupal Dev,

Ferrer,

Okawa

2024

J. Cosmol. Astropart. Phys.

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“…In addition, the ratio is also limited by the physical scale of the experiment, such as the bore size of the magnet, which constrains the overall size of 𝜌 𝑐 . we conservatively set 𝜌 𝑚 /𝜌 𝑐 = 1/2 to match the relative size of the HAYSTAC experiment [20].…”

Section: Jinst 18 P07017mentioning

confidence: 99%

“…We now define excessive mode crossings as more than 15% of the total cavity tuning range. For example, a haloscope experiment such as the HAYSTAC has a tuning range of about 2 GHz, and 15% of that corresponds to one major mode crossing every 300 MHz.1 Taking a cavity with a loaded quality factor of 𝑄 𝐿 ∼ 5000 and a bandwidth of Δ𝜈 ∼ 1 MHz as an example [20], this requires tuning about 300 times the cavity bandwidth before hitting a mode crossing, which is a reasonable goal for a practical experiment that wants to cover a wide range. This can be written as…”

Section: Jinst 18 P07017mentioning

confidence: 99%

On the use of dielectric elements in axion searches with microwave resonant cavities

et al. 2023

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This study explores the primary effects of dielectric materials in a resonant cavity-based search for axion dark matter. While dielectrics prove beneficial in numerous cases, their incorporation may lead to less-than-optimal performance, especially for the lowest TM mode. Additionally, the stronger confinement of the electric field inside the dielectrics can exacerbate mode mixings, in particular for higher-order modes. Case studies have been carried out using a combination of analytical solutions and numerical simulations. The findings indicate dielectric cavities employing the TM010 mode experience a significant reduction in sensitivity when compared to a similar search conducted in a cavity at equivalent frequency using no dielectrics.

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“…On the contrary, there is no a priori relation between mass and coupling strength for ALPs, making the potential parameter space broader [28,29]. Many experiments world wide are actively searching for these particles using resonant cavity haloscopes [30,31] or large-scale helioscopes [32] to detect WISPs based on cosmological and astrophysical sources. Additionally, laboratory-based experiments employing nuclear magnetic resonant precision magnetometers searching for EDM interactions with ALPs [33,34], a broadband/resonant approach with a toroidal magnet looking for an axion-induced magnetic field [35], or employing search methods based on the concept of 'light shining through a wall' [36,37] or the search for a 'fifth force' [38,39], have also been looking for WISPs in the past few decades.…”

Section: Introductionmentioning

confidence: 99%

Search for an interaction mediated by axion-like particles with ultracold neutrons at the PSI

Ayres,

Bison,

Bodek

et al. 2023

New J. Phys.

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We report on a search for a new, short-range, spin-dependent interaction using a modified version of the experimental apparatus used to measure the permanent neutron electric dipole moment at the Paul Scherrer Institute. This interaction, which could be mediated by axion-like particles, concerned the unpolarized nucleons (protons and neutrons) near the material surfaces of the apparatus and polarized ultracold neutrons stored in vacuum. The dominant systematic uncertainty resulting from magnetic-field gradients was controlled to an unprecedented level of approximately 4 pT cm−1 using an array of optically-pumped cesium vapor magnetometers and magnetic-field maps independently recorded using a dedicated measurement device. No signature of a theoretically predicted new interaction was found, and we set a new limit on the product of the scalar and the pseudoscalar couplings g s g p λ 2 < 8.3 × 10 − 28 m2 (95% C.L.) in a range of 5 µm < λ < 25 mm for the monopole–dipole interaction. This new result confirms and improves our previous limit by a factor of 2.7 and provides the current tightest limit obtained with free neutrons.

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New results from HAYSTAC’s phase II operation with a squeezed state receiver

Cited by 23 publications

References 59 publications

On the Galactic radio signal from stimulated decay of axion dark matter

On the Galactic radio signal from stimulated decay of axion dark matter

On the use of dielectric elements in axion searches with microwave resonant cavities

Search for an interaction mediated by axion-like particles with ultracold neutrons at the PSI

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