Abstract
Dark matter searches have been ongoing for three decades; the lack of a positive discovery of the main candidate, the WIMP, after dedicated efforts, has put axions and axion-like particles in the spotlight. The three main techniques employed to search for them complement each other well in covering a wide range in the parameter space defined by the axion decay constant and the axion mass. The International AXion Observatory (IAXO) is an international collaboration planning to build the fourth generation axion helioscope, with an unparalleled expected sensitivity and discovery potential. The distinguishing characteristic of IAXO is that it will feature a magnet that is designed to maximise the relevant parameters in sensitivity and which will be equipped with X-ray focusing devices and detectors that have been developed for axion physics. In this paper, we review aspects that motivate IAXO and its prototype, BabyIAXO, in the axion, and ALPs landscape. As part of this Special Issue, some emphasis is given on Spanish participation in the project, of which CAPA (Centro de Astropartículas y Física de Altas Energías of the Universidad de Zaragoza) is a strong promoter.
Highlights
Introduction into AxionPhysics with (Baby)International AXion Observatory (IAXO).The last century marked an era for the field of particle physics; did it offer the technological progress necessary to develop new detection techniques, it brought the acceptance of special relativity and quantum mechanics as a basis to construct new physics models
In the second part of this document, we present the initiative from the IAXO collaboration to build the generation axion helioscope, focusing on the different components of the instrument (Section 5) and the Spanish leading role and contribution to the experiment (Section 6)
A star is a rich particle physics laboratory where we find many different physics processes and interactions where axions could be produced inside the stellar medium [38]
Summary
The axion is a hypothetical particle that emerged as a natural solution to the strong. 0.2sys ) × 10−26 e·cm, its corresponding upper limit dn < 1.8 × 10−26 e·cm [6], and a recent calculation in QCD, |dn | < 10−15 · θ e·cm [7] In principle, this phase could take any value between 0 and 2π, since it is produced adding up QCD contributions of different nature, arising the question why this phase would have chosen a value such that the strong. The Peccei–Quinn mechanism to restore CP conservation in the strong sector [8,9] led soon into an interesting outcome—the axion—arising naturally as a dynamic solution to the fine tuning problem of the θ parameter [10,11], effectively, θ is replaced by θ + a/ f a , where a is the axion field, and f a is the energy scale at which the field symmetry would be spontaneously broken
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