Axion Dark Matter Search around 4.55 $μ$eV with Dine-Fischler-Srednicki-Zhitnitskii Sensitivity

Yi, Andrew K.; Ahn, Saebyeok; Kutlu, Çağlar; Kim, JinMyeong; Ko, B. R.; Ivanov, B. I.; Byun, HeeSu; Loo, Arjan F. van; Park, SeongTae; Jeong, J. H.; Kwon, Ohjoon; Nakamura, Y.; Uchaikin, S.; Choi, Jihoon; Lee, Soohyung; Lee, Myeong Jae; Shin, Yun Chang; Kim, Jinsu; Lee, Doyu; Ahn, Danho; Bae, Sungjae; Lee, Jiwon; Kim, Young-Geun; Gkika, Violeta; Lee, Ki Woong; Oh, Seonjeong; Seong, Taehyeon; Kim, Dong-Min; Chung, Woohyun; Matlashov, Andrei; Youn, S. W.; Semertzidis, Yannis K.

doi:10.48550/arxiv.2210.10961

Cited by 6 publications

(16 citation statements)

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“…Comparing with the sensitivity prospects of axion dark matter experiments (axion haloscopes) shown in Fig. 4, we conclude: ADMX [36], BabyIAXO-RADES [37], CAPP [38], FLASH [39], or DMRadio [40] have good prospects to smash SM*A*S*H by discovering an axion with a mass below 26 micro-eV!…”

Section: Pos(cosmicwispers)003mentioning

confidence: 69%

Prospects to scrutinise or smash SMAS*H

Ringwald

2024

Proceedings of 1st General Meeting and 1st Training School of the COST Action COSMIC WSIPers — PoS(COSMICWISPers)

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is an extension of the Standard Model of particle physics which has just the minimal number of fields in order to solve six puzzles of particle physics and cosmology in one smash: vacuum stability, inflation, baryon asymmetry, neutrino masses, strong CP, and dark matter. The parameters of SM*A*S*H are constrained by symmetries and requirements to solve these puzzles. This provides various firm predictions for observables which can be confronted with experiments. We discuss the prospects and timeline to scrutinise or smash SM*A*S*H by cosmic microwave background polarisation experiments, axion haloscopes, and future space-borne gravitational wave detectors.

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Section: Pos(cosmicwispers)003mentioning

confidence: 69%

Prospects to scrutinise or smash SMAS*H

Ringwald

2024

Proceedings of 1st General Meeting and 1st Training School of the COST Action COSMIC WSIPers — PoS(COSMICWISPers)

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“…The solid and dashed parts of these lines respectively show the current and projected sensitivity of searches for flavor-violating axion couplings. The region where the QCD axion can make up the observed dark matter abundance is unshaded (see table 1) [19][20][21][22] Also shown are various other constraints arising from terrestrial experiments [68][69][70][71][72][73][74][75][76][77][78] (blue) and astrophysical observations [79,80] (green). these generally flavor-violating interactions.…”

Section: Discussionmentioning

confidence: 99%

The flavor of QCD axion dark matter

Alonso-Álvarez

Cline

Xiao

2023

J. High Energ. Phys.

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We argue that demanding a consistent cosmological history, including the absence of domain walls and strongly interacting relics at the Peccei-Quinn scale, singles out two concrete realizations of hadronic QCD axions as viable dark matter models. These realizations generally feature flavor-violating axion couplings to Standard Model quarks that are unsuppressed at low energies. As a consequence, experiments looking for flavor-violating hadronic processes involving the axion can be sensitive probes of QCD axion dark matter models. In particular, we show that the NA62 and KOTO experiments could detect the K → π + a decay for axions consistent with the observed dark matter abundance via the post-inflationary misalignment mechanism.

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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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Axion Dark Matter Search around 4.55 $μ$eV with Dine-Fischler-Srednicki-Zhitnitskii Sensitivity

Cited by 6 publications

References 0 publications

Prospects to scrutinise or smash SMAS*H

Prospects to scrutinise or smash SMAS*H

The flavor of QCD axion dark matter

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

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Axion Dark Matter Search around 4.55 $μ$eV with Dine-Fischler-Srednicki-Zhitnitskii Sensitivity

Cited by 6 publications

References 0 publications

Prospects to scrutinise or smash SM*A*S*H

Prospects to scrutinise or smash SM*A*S*H

The flavor of QCD axion dark matter

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

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Prospects to scrutinise or smash SMAS*H

Prospects to scrutinise or smash SMAS*H