Photon-axion conversion, magnetic field configuration, and polarization of photons

Masaki, Emi; Aoki, Arata; Soda, Jiro

doi:10.1103/physrevd.96.043519

Cited by 40 publications

(17 citation statements)

References 48 publications

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“…where A x (y) and A z describe the photon linear polariza-tion amplitudes along the x and z axis, respectively, a(y) is the ALP amplitude. From the Lagrangian of photon-ALP system, we can derive the beam propagation equation for ultra-relativistic ALPs [43,47,59,60] i…”

Section: Alp (Axion-like Particle)-photon Oscillationmentioning

confidence: 99%

Testing the CIBER cosmic infrared background measurements and axionlike particles with observations of TeV blazars

et al. 2020

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The first measurements from the CIBER experiment of extragalactic background light (EBL) in near-infrared (NIR) band exhibit a higher intensity than those inferred through γ-ray observations. Recent theoretical-EBL intensities are typically consistent with the very high energy (VHE) γ-ray observations. Yet, it is possible that the excess NIR radiation is a new component of EBL and not in tension with the TeV spectra of distant blazars, since the hypothetical axion-like particle (ALP) may lead to a reduced opacity of the Universe for VHE γ-rays. In order to probe whether the excess component arises mainly from EBL, thirteen observed spectra in high energy and VHE ranges from ten distant TeV BL Lac objects are fitted by four theoretical spectra which involve theoretical EBL (Gilmore ), Gilmore's EBL model including photon/ALP coupling, Gilmore's EBL with CIBER excess and the latter including photon/ALP coupling respectively. We find the goodness of fit for the model with CIBER excess can be improved with a significance of 7.6 σ after including the photon/ALP coupling; Thus, the ALP/photon mixing mechanism can effectively alleviate the tension; However, the Gilmore EBL model, on the whole, is more compatible with the observed spectra compared to those with ALP, although individual blazars such as PKS 1424+240 and 1ES 1101-232 prefer the ALP-model. Our results suggest that the recent EBL models can solely explain the VHE γ-ray observations, and assuming the existence of the ALP to alleviate the tension is not required in a statistical sense, thus the excess over the EBL models is less likely to be a new EBL component. * EBL intensities (for reviews see e.g. Refs. [1,16,17]) and test the empirical EBL models, e.g. Refs. [8][9][10][11][12][13], by comparing the difference between the assumed-intrinsic spectra and the observed one. Thanks to the discovery of more and more distant Tev blazars, several groups have detected this imprint, e.g. Refs. [15,18,19], and found the intensities were near the galaxy-count lower limits.The spectra of a few individual blazars such as PKS1424+240 appear to be unexpectedly hard [34]. Furthermore, hints for a reduced gamma-ray opacity in the form of a pair-production anomaly [20] (i.e., VHE γ-ray observations require an EBL level below the lower limits from galaxy counts), or unusual redshift-dependent intrinsic (after correction for EBL absorption) spectral hardening found in large samples, have been claimed by several authors [21][22][23][24]. However, no significant and systematic anomalies on the entire sample were revealed by recent systematic studies of spectra fitted with recent theoretical EBL absorption on large samples of VHE blazars, see e.g., 33,34]. The intensities of these recent EBL models (e.g. Franceschini 2008 [8], Dominguez 2011 [9], Kneiske 2010 [10], Finke 2010 [11], Gilmore 2012 [12], Stecker 2016 [13]) are close to that from the galaxy counts. At present, many EBL measurements inferred by γ-ray observations reveal that its intensities are generally consistent with ...

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Section: Alp (Axion-like Particle)-photon Oscillationmentioning

confidence: 99%

Testing the CIBER cosmic infrared background measurements and axionlike particles with observations of TeV blazars

et al. 2020

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“…Some limits were derived using gamma-ray observations [327,[332][333][334], but much of the parameter space is excluded due to observations of photons in wavelengths other than gamma rays. Interestingly, some works have been obtaining combined limits on IGMFs and ALPs together [335]. For reviews on the status of the field, see, e.g., Refs.…”

Section: Other Propagation Phenomenamentioning

confidence: 99%

The Gamma-ray Window to Intergalactic Magnetism

Batista

Saveliev

2021

Universe

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One of the most promising ways to probe intergalactic magnetic fields (IGMFs) is through gamma rays produced in electromagnetic cascades initiated by high-energy gamma rays or cosmic rays in the intergalactic space. Because the charged component of the cascade is sensitive to magnetic fields, gamma-ray observations of distant objects such as blazars can be used to constrain IGMF properties. Ground-based and space-borne gamma-ray telescopes deliver spectral, temporal, and angular information of high-energy gamma-ray sources, which carries imprints of the intervening magnetic fields. This provides insights into the nature of the processes that led to the creation of the first magnetic fields and into the phenomena that impacted their evolution. Here we provide a detailed description of how gamma-ray observations can be used to probe cosmic magnetism. We review the current status of this topic and discuss the prospects for measuring IGMFs with the next generation of gamma-ray observatories.

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“…The existence of φγγ vertex leads to a two-photon decay of φ, as well as to effects of φγ conversion [64] like axion-photon conversion in magnetic field (see e.g. [65] for review and references). The principles of experimental search for axion by "light shining through walls" effects are based on such a conversion [66].…”

Section: Pseudo Nambu-goldstone Fieldmentioning

confidence: 99%

Cosmoparticle physics of dark matter

Khlopov

2019

EPJ Web Conf.

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The lack of confirmation for the existence of supersymmetric particles and Weakly Interacting Massive Particles (WIMPs) appeals to extension of the field of studies of the physical nature of dark matter, involving nonsupersymmetric and non-WIMP solutions. We briefly discuss some examples of such candidates in their relationship with extension of particle symmetry and pattern of symmetry breaking. We specify in the example of axion-like particles nontrivial features of cosmological reflection of the structure and pattern of Peccei-Quinn-like symmetry breaking. The puzzles of direct and indiect dark matter searches can find solution in the approach of composite dark matter. The advantages and open problems of this approach are specified. We note that detailed analysis of cosmological consequences of any extension of particle model that provides candidates for dark matter inevitably leads to nonstandard features in the corresponding cosmological scenario. It makes possible to use methods of cosmoparticle physics to study physical nature of the dark matter in the combination of its physical, astrophysical and cosmological signatures. *

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Photon-axion conversion, magnetic field configuration, and polarization of photons

Cited by 40 publications

References 48 publications

Testing the CIBER cosmic infrared background measurements and axionlike particles with observations of TeV blazars

Testing the CIBER cosmic infrared background measurements and axionlike particles with observations of TeV blazars

The Gamma-ray Window to Intergalactic Magnetism

Cosmoparticle physics of dark matter

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