Search for Sub-eV Mass Solar Axions by the CERN Axion Solar Telescope with<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>He</mml:mi><mml:mprescripts/><mml:none/><mml:mn>3</mml:mn></mml:mmultiscripts></mml:math>Buffer Gas

Arık, M.; Aune, S.; Barth, K.; Белов, А. С.; Borghi, S.; Bräuninger, H.; Cantatore, G.; Carmona, J. M.; Çetin, S. A.; Collar, J. I.; Dafní, T.; Davenport, M.; Eleftheriadis, C.; Elías, Nicolás; Ezer, Cemile; Fanourakis, G.; Ferrer‐Ribas, E.; Friedrich, Péter; Galán, J.; Garcı́a, Juan Antonio; Gardikiotis, A.; Gazis, E. N.; Geralis, T.; Giomataris, I.; Gninenko, S.; Gómez, H.; Gruber, E.; Guthörl, T.; Hartmann, R.; Haug, F.; Hasinoff, M.; Hoffmann, D. H. H.; Iguaz, F.J.; Irastorza, I.G.; Jacoby, J.; Jakovčić, K.; Karuza, M.; Königsmann, K.; Kotthaus, R.; Krčmar, M.; Kuster, M.; Lakić, B.; Laurent, J.; Liolios, A.; Ljubičić, A.; Lozza, V.; Lütz, G.; Luzón, G.; Morales, J.; Niinikoski, T.; Nordt, Annika; Papaevangelou, T.; Pivovaroff, M. J.; Raffelt, Georg G.; Rashba, T. I.; Riege, H.; Rodríguez, A. Soto; Rosu, M.; Ruz, J.; Savvidis, I.; Silva, P. S.; Solanki, S. K.; Stewart, L.; Tomás, A.; Tsagri, M.; Bibber, K. van; Vafeiadis, T.; Villar, J.A.; Vogel, Julia K.; Yildiz, S.C.; Zioutas, K.

doi:10.1103/physrevlett.107.261302

Cited by 144 publications

(115 citation statements)

References 35 publications

(59 reference statements)

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“…It uses a Large Hadron Collider (LHC) dipole prototype magnet with a magnetic field of up to 9 T over a length of 9.3 m and an aperture of 2 × 15 cm 2 [27], that is able to follow the Sun for ∼3 hours per day using an elevation and azimuth drive. During its 10-year experimental program [25,[28][29][30][31][32], CAST has seen no signal of solar axions, and a number of upper limits on the photon-axion coupling g aγ at the level of 10 −10 GeV −1 for axion masses up to ∼1 eV have been derived. It is the most stringent experimental bound in most of this axion mass range.…”

Section: Micromegas Chambers In the Search For Solar Axionsmentioning

confidence: 99%

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Irastorza

Aznar

Castel

et al. 2016

J. Cosmol. Astropart. Phys.

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Abstract. As part of the T-REX project, a number of R&D and prototyping activities have been carried out during the last years to explore the applicability of gaseous Time Projection Chambers (TPCs) with Micromesh Gas Structures (Micromegas) in rare event searches like double beta decay, axion research and low-mass WIMP searches. While in the companion paper we focus on double beta decay, in this paper we focus on the results regarding the search for dark matter candidates, both axions and WIMPs.

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Section: Micromegas Chambers In the Search For Solar Axionsmentioning

confidence: 99%

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Irastorza

Aznar

Castel

et al. 2016

J. Cosmol. Astropart. Phys.

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“…The data analysis follows similar previous analyses of CAST data [14][15][16] . We define an unbinned likelihood function…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

New CAST limit on the axion–photon interaction

2017

Nature Phys

843

709

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Hypothetical low-mass particles, such as axions, provide a compelling explanation for the dark matter in the universe. Such particles are expected to emerge abundantly from the hot interior of stars. To test this prediction, the CERN Axion Solar Telescope (CAST) uses a 9 T refurbished Large Hadron Collider test magnet directed towards the Sun. In the strong magnetic field, solar axions can be converted to X-ray photons which can be recorded by X-ray detectors. In the 2013-2015 run, thanks to low-background detectors and a new X-ray telescope, the signal-to-noise ratio was increased by about a factor of three. Here, we report the best limit on the axion-photon coupling strength (0.66 × 10 −10 GeV −1 at 95% confidence level) set by CAST, which now reaches similar levels to the most restrictive astrophysical bounds.A dvancing the low-energy frontier is a key endeavour in the worldwide quest for particle physics beyond the standard model and in the effort to identify dark matter 1,2 . Nearly massless pseudoscalar bosons, often generically called axions, are particularly promising because they appear in many extensions of the standard model. They can be dark matter in the form of classical field oscillations that were excited in the early universe, notably by the re-alignment mechanism 3 . One particularly well motivated case is the quantum chromodynamics (QCD) axion, the eponym for all such particles. The existence of this new lowmass boson follows from the Peccei-Quinn mechanism as an explanation why QCD is perfectly time-reversal invariant within current experimental precision 3 .Axions were often termed 'invisible' because of their extremely feeble interactions, yet they are the target of a fast-growing international landscape of experiments. Numerous existing and foreseen projects assume that axions are the galactic dark matter and use a variety of techniques that are sensitive to different interaction channels and optimal in different mass ranges 4 . Independently of the dark-matter assumption, one can search for new forces mediated by these low-mass bosons 5 or the back-reaction on spinning black holes (superradiance) 6 . Stellar energy-loss arguments provide restrictive limits that can guide experimental efforts, and in some cases may even suggest new loss channels 3,7,8 .The least model-dependent search strategies use the production and detection of axions and similar particles by their generic twophoton coupling. It is given by the vertex L aγ = −(1/4) g aγ F µν F µν a = g aγ E · B a, where a is the axion field, F the electromagnetic field-strength tensor, and g aγ a coupling constant of dimension (energy) −1 . Notice that we use natural units with = c = k B = 1. This vertex enables the decay a → γ γ , the Primakoff production in stars-that is, the γ → a scattering in the Coulomb fields of charged particles in the stellar plasma-and the coherent conversion a ↔ γ in laboratory or astrophysical B-fields 9,10 .The helioscope concept, in particular, uses a dipole magnet directed at the Sun to convert axions to...

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“…The QCD axion has only one free parameter, f a , in such constraints and occupies a line in the mass-coupling plane, but constraints to general axion-like particles apply to regions of this parameter space. Current experiments include ADMX [89] (haloscope), CAST [90] (helioscope), and ALPS-I [91] (LSW).…”

Section: Direct and Indirect Detection Of Axions And Astrophysicalmentioning

confidence: 99%

A search for ultralight axions using precision cosmological data

et al. 2015

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Ultralight axions (ULAs) with masses in the range 10 −33 eV ≤ m a ≤ 10 −20 eV are motivated by string theory and might contribute to either the dark-matter or dark-energy densities of the Universe. ULAs could suppress the growth of structure on small scales, lead to an altered integrated Sachs-Wolfe effect on cosmic microwave-background (CMB) anisotropies, and change the angular scale of the CMB acoustic peaks. In this work, cosmological observables over the full ULA mass range are computed and then used to search for evidence of ULAs using CMB data from the Wilkinson Microwave Anisotropy Probe (WMAP), Planck satellite, Atacama Cosmology Telescope, and South Pole Telescope, as well as galaxy clustering data from the WiggleZ galaxy-redshift survey. In the mass range 10 −32 eV ≤ m a ≤ 10 −25.5 eV, the axion relicdensity Ω a (relative to the total dark-matter relic density Ω d ) must obey the constraints Ω a =Ω d ≤ 0.05 and Ω a h 2 ≤ 0.006 at 95% confidence. For m a ≳ 10 −24 eV, ULAs are indistinguishable from standard cold dark matter on the length scales probed, and are thus allowed by these data. For m a ≲ 10 −32 eV, ULAs are allowed to compose a significant fraction of the dark energy.

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Search for Sub-eV Mass Solar Axions by the CERN Axion Solar Telescope withHe3Buffer Gas

Cited by 144 publications

References 35 publications

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

New CAST limit on the axion–photon interaction

A search for ultralight axions using precision cosmological data

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