Search for chameleons with CAST

Anastassopoulos, V.; Arık, M.; Aune, S.; Barth, K.; Белов, А. С.; Bräuninger, H.; Cantatore, G.; Carmona, J. M.; Çetin, S. A.; Christensen, F.; Collar, J. I.; Dafní, T.; Davenport, M.; Desch, K.; Dermenev, A.; Eleftheriadis, C.; Fanourakis, G.; Ferrer‐Ribas, E.; Friedrich, Péter; Galán, J.; Garcı́a, Juan Antonio; Gardikiotis, A.; Garza, J.G.; Gazis, E. N.; Geralis, T.; Giomataris, I.; Hailey, Charles J.; Haug, F.; Hasinoff, M.; Hoffmann, D. H. H.; Iguaz, F.J.; Irastorza, I.G.; Jacoby, J.; Jakobsen, Anders Clemen; Jakovčić, K.; Kamiński, J.; Karuza, M.; Kavuk, Mehmet; Krčmar, M.; Krieger, C.; Krüger, A.; Lakić, B.; Laurent, J.; Liolios, A.; Ljubičić, A.; Luzón, G.; Neff, S.; Ortega, I.; Papaevangelou, T.; Pivovaroff, M. J.; Raffelt, Georg G.; Riege, H.; Rosu, M.; Ruz, J.; Savvidis, I.; Solanki, S. K.; Vafeiadis, T.; Villar, J.A.; Vogel, Julia K.; Yildiz, S.C.; Zioutas, K.; Brax, Ph.; Lavrentyev, I.; Upadhye, Amol

doi:10.1016/j.physletb.2015.07.049

Cited by 43 publications

(42 citation statements)

References 46 publications

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“…The effect of DE on cosmological scales is studied by measuring the redshift-distance relation using supernovae, baryon acoustic oscillations, the matter power spectrum and the cosmic microwave background, as well as gravitational lensing [44]. On microscopic scales, DE is probed by laboratory experiments searching for additional gravitational forces that would lead to deviations from the 1/r 2 law [45][46][47][48][49][50][51][52][53]. Multi-messenger astronomical observations also provide important information for understanding the nature of DE [54][55][56].…”

Section: Introductionmentioning

confidence: 99%

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Constraints on mediator-based dark matter and scalar dark energy models using $$ \sqrt{s} $$ = 13 TeV pp collision data collected by the ATLAS detector

Aaboud¹,

Aad²,

Abbott³

et al. 2019

J. High Energ. Phys.

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Constraints on mediator-based dark matter and scalar dark energy models using √ s = 13 TeV p p collision data collected by the ATLAS detectorThe ATLAS Collaboration Constraints on selected mediator-based dark matter models and a scalar dark energy model using up to 37 fb −1 √ s = 13 TeV pp collision data collected by the ATLAS detector at the LHC during 2015-2016 are summarised in this paper. The results of experimental searches in a variety of final states are interpreted in terms of a set of spin-1 and spin-0 single-mediator dark matter simplified models and a second set of models involving an extended Higgs sector plus an additional vector or pseudo-scalar mediator. The searches considered in this paper constrain spin-1 leptophobic and leptophilic mediators, spin-0 colour-neutral and colour-charged mediators and vector or pseudo-scalar mediators embedded in extended Higgs sector models. In this case, also √ s = 8 TeV pp collision data are used for the interpretation of the results. The results are also interpreted for the first time in terms of light scalar particles that could contribute to the accelerating expansion of the universe (dark energy).

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Section: Introductionmentioning

confidence: 99%

“…on pp 3,15,16,. 18,45,47). [21] ATLAS Collaboration, Search for dark matter at √ s = 13 TeV in final states containing an energetic photon and large missing transverse momentum with the ATLAS detector, Eur.…”

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confidence: 99%

Constraints on mediator-based dark matter and scalar dark energy models using $$ \sqrt{s} $$ = 13 TeV pp collision data collected by the ATLAS detector

Aaboud¹,

Aad²,

Abbott³

et al. 2019

J. High Energ. Phys.

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“…The CAST data were also interpreted in terms of other assumed axion production channels in the Sun [20][21][22] . Moreover, CAST constraints on other low-mass bosons include chameleons 23 and hidden photons 24 .During this long experimental programme, CAST has used a variety of detection systems at both magnet ends, including a multiwire time projection chamber 25 , several Micromegas detectors 26 , a low-noise charged coupled device attached to a spare X-ray telescope (XRT) from the ABRIXAS X-ray mission 27 , a γ -ray calorimeter 21 , and a silicon drift detector 23 .In the latest data-taking campaign (2013)(2014)(2015), CAST has returned to evacuated pipes, with an improvement in the sensitivity to solar axions of about a factor of three in signal-tonoise ratio over a decade ago, thanks to the development of novel detection systems-notably new Micromegas detectors with lower background levels, as well as a new XRT built specifically for axion searches. These developments are also part of the activities to define the detection technologies suitable for the proposed much larger next-generation axion helioscope IAXO 28 .…”

mentioning

confidence: 99%

“…During this long experimental programme, CAST has used a variety of detection systems at both magnet ends, including a multiwire time projection chamber 25 , several Micromegas detectors 26 , a low-noise charged coupled device attached to a spare X-ray telescope (XRT) from the ABRIXAS X-ray mission 27 , a γ -ray calorimeter 21 , and a silicon drift detector 23 .…”

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confidence: 99%

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New CAST limit on the axion–photon interaction

2017

Nature Phys

836

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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Solar Production of Ultralight Bosons

Vogel

Irastorza

2022

The Search for Ultralight Bosonic Dark Matter

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This chapter will spotlight axions produced in the core of the Sun. A first focus will be put on the production mechanism for axions in the solar interior through coupling of axions to photons via the Primakoff effect as well as their interactions with electrons. In addition to the axion production, the axion-to-photon conversion probability is a crucial quantity for solar axion searches (also referred to as helioscopes) and determines the expected number of photons from solar axion conversion that are detectable in a ground-based search. After these basic considerations, the helioscope concept will be detailed, and past, current, and future experimental realizations of axion helioscopes will be discussed. This includes the analysis used to aim at axion detection and upper limit calculations in case no signal above background is detected in experimental data. For completeness, alternative approaches other than traditional helioscopes to search for solar axions are discussed.

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Search for chameleons with CAST

Cited by 43 publications

References 46 publications

Constraints on mediator-based dark matter and scalar dark energy models using $$ \sqrt{s} $$ = 13 TeV pp collision data collected by the ATLAS detector

Constraints on mediator-based dark matter and scalar dark energy models using $$ \sqrt{s} $$ = 13 TeV pp collision data collected by the ATLAS detector

New CAST limit on the axion–photon interaction

Solar Production of Ultralight Bosons

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