First results on the search for chameleons with the KWISP detector at CAST

Cuendis, S. Arguedas; Baier, Joseph G.; Barth, K.; Baum, Sebastian; Bayirli, A.; Белов, А. С.; Bräuninger, H.; Cantatore, G.; Carmona, J. M.; Castel, J.; Çetin, S. A.; Dafní, T.; Davenport, M.; Dermenev, A.; Desch, K.; Döbrich, Babette; Fischer, H.; Funk, W.; Garcı́a, Juan Antonio; Gardikiotis, A.; Garza, J.G.; Gninenko, S.; Hasinoff, M.; Hoffmann, D. H. H.; Iguaz, F.J.; Irastorza, I.G.; Jakovčić, K.; Kamiński, J.; Karuza, M.; Krieger, C.; Lakić, B.; Laurent, J.; Luzón, G.; Maroudas, Marios; Miceli, L.; Neff, S.; Ortega, I.; Özbey, A.; Pivovaroff, M. J.; Rosu, M.; Ruz, J.; Ruiz-Choliz, Elisa; Schmidt, Sebastian; Schümann, M.; Semertzidis, Y. K.; Solanki, S. K.; Stewart, L.; Tsagris, I.; Vafeiadis, T.; Vogel, Julia K.; Vretenar, Mario; Yildiz, S.C.; Zioutas, K.

doi:10.1016/j.dark.2019.100367

Cited by 16 publications

(7 citation statements)

References 24 publications

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“…Demanding that solar chameleons fit the XENON1T signal, and combining the relation in Eq. ( 16) and the upper limit of β γ < 10 11 from CAST [51] sets an upper limit on M e 10 MeV. In other words, if M e 10 MeV, for any allowed value of β γ the event rate will be completely dominated by B 0 , and we will find ourselves along the plateau for large negative values of log 10 β eff in Fig.…”

Section: Resultsmentioning

confidence: 92%

“…We impose flat priors on log 10 β γ ∈ [0; 11], log 10 (M γ /keV) ∈ [0; 25], log 10 β e ∈ [1; 2], and log 10 (M e /keV) ∈ [0; 25]. For β γ , the upper prior edge is motivated by the latest results from the Kinetic Weakly Interacting Slim Particles (KWISP) detector on the CAST axion search experiment at CERN, which finds β γ < 10 11 [51], whereas the lower prior edge is arbitrary (we have checked that extending it to lower values does not qualitatively affect our final results). Due to the weak sensitivity of the XENON1T measurements to β e , we have chosen a narrow prior for this parameter.…”

Section: Discussionmentioning

confidence: 99%

“…This possibility opens up yet another exciting avenue for directly detecting DE fluctuations: DE particles produced in the solar tachocline could be observed in dark matter (DM) direct detection experiments. To date, searches for DE-like particles in direct detection experiments have mostly focused on axion-specific experiments such as the CERN Axion Solar Telescope (CAST) [48][49][50][51] and the Axion Dark Matter Experiment (ADMX) [52]. Other detection techniques currently being considered are at different stages of realisation, or have started to gather data [53][54][55][56][57][58][59].…”

Section: Introductionmentioning

confidence: 99%

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Direct detection of dark energy: the XENON1T excess and future prospects

Vagnozzi,

Visinelli,

Brax

et al. 2021

Preprint

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We explore the prospects for direct detection of dark energy by current and upcoming terrestrial dark matter direct detection experiments. If dark energy is driven by a new light degree of freedom coupled to matter and photons then dark energy quanta are predicted to be produced in the Sun. These quanta free-stream towards Earth where they can interact with Standard Model particles in the detection chambers of direct detection experiments, presenting the possibility that these experiments could be used to test dark energy. Screening mechanisms, which suppress fifth forces associated with new light particles, and are a necessary feature of many dark energy models, prevent production processes from occurring in the core of the Sun, and similarly, in the cores of red giant, horizontal branch, and white dwarf stars. Instead, the coupling of dark energy to photons leads to production in the strong magnetic field of the solar tachocline via a mechanism analogous to the Primakoff process. This then allows for detectable signals on Earth while evading the strong constraints that would typically result from stellar probes of new light particles. As an example, we examine whether the electron recoil excess recently reported by the XENON1T collaboration can be explained by chameleon-screened dark energy, and find that such a model is preferred over the background-only hypothesis at the 2.0σ level, in a large range of parameter space not excluded by stellar (or other) probes. This raises the tantalizing possibility that XENON1T may have achieved the first direct detection of dark energy. Finally, we study the prospects for confirming this scenario using planned future detectors such as XENONnT, PandaX-4T, and LUX-ZEPLIN.

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Section: Resultsmentioning

confidence: 92%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Direct detection of dark energy: the XENON1T excess and future prospects

Vagnozzi,

Visinelli,

Brax

et al. 2021

Preprint

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“…symmetrons [74]. Particularly relevant is the case of chameleons, that have been searched for as a byproduct of axion experiments [75][76][77][78].…”

Section: Other Cosmological Phenomenology and Constraints On Axion/al...mentioning

confidence: 99%

An introduction to axions and their detection

Irastorza

2022

SciPost Phys. Lect. Notes

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In these notes I try to introduce the reader to the topic of axions: their theoretical motivation and expected phenomenology, their role in astrophysics and as a dark matter candidate, and the experimental techniques to detect them. Special emphasis is made in this last point, for which a relatively updated review of worldwide efforts and future prospects is made. The material is intended as an introduction to the topic, and it was prepared as lecture notes for Les Houches summer school 2021. Abundant references are included to direct the reader to deeper insight on the different aspects of axion physics.

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“…Some examples are quintessence fields [54][55][56][57], chameleons [58][59][60], galileons [61], symmetrons [62]. Particularly relevant is the case of chamaleons, that have been searched for as byproduct of axion experiments [63][64][65][66].…”

Section: Other Cosmological Phenomenology and Constraints On Axion/al...mentioning

confidence: 99%

An introduction to axions and their detection

Irastorza

2021

Preprint

View full text Add to dashboard Cite

In these notes I try to introduce the reader to the topic of axions: their theoretical motivation and expected phenomenology, their role in astrophysics and as dark matter candidate, and the experimental techniques to detect them. Special emphasis is made in this last point, for which a relatively updated review of worldwide efforts and future prospects is made. The material is intended as an introduction to the topic, and it was prepared as lecture notes for Les Houches summer school 2021. Abundant references are included to direct the reader to deeper insight on the different aspects of axion physics.

show abstract

First results on the search for chameleons with the KWISP detector at CAST

Cited by 16 publications

References 24 publications

Direct detection of dark energy: the XENON1T excess and future prospects

Direct detection of dark energy: the XENON1T excess and future prospects

An introduction to axions and their detection

An introduction to axions and their detection

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