ORIGINAL RESEARCH article
Front. Detect. Sci. Technol.
Sec. Detector Physics
Volume 3 - 2025 | doi: 10.3389/fdest.2025.1580297
This article is part of the Research TopicFundamentals of luminescence and electroluminescence in particle detection technologies relying on noble-gas mediaView all 5 articles
Near Infrared Cathodoluminescence of Xe 2 Excimers in Dense Gaseous Mixtures
Provisionally accepted- 1Department of Physics and Astronomy, School of Sciences, University of Padua, Padua, Veneto, Italy
- 2National Institute of Nuclear Physics of Padova, Padova, Italy
- 3ParisTech Chemistry - PSL University, Paris, Ile-de-France, France
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We report new spectroscopic measurements of the near infrared (NIR) fluorescence band of electron-beam excited Xe 2 excimers as a function of the gas density in several gaseous mixtures of different Xe concentrations at room temperature. We have used He, Ar, and N 2 as buffer gases, the Xe concentration in the mixtures ranging from about 8 % up to 80 %. The investigated density range extends up to 10 times the density N ig of the ideal gas at standard temperature and pressure (N ig ≈ 2.5 × 10 25 m -3 ). In all mixtures we have observed that the wavelength of the centroid of the infrared excimer band is shifted towards longer wavelenghts as the gas density is increased, in a similar way as it was originally observed in pure Xe gas and in an Ar-Xe mixture.The strength of the redshift depends on the Xe concentration in the mixture and on the nature of the buffer gas and is very well rationalized by taking into account both the classical dielectric screening effect due to the gaseous environment and the density-dependent quantum shift of the energy of the optically active electron in the Xe 2 molecule, provided that the contribution of the two gaseous species in the mixture is weighted by applying the laws of ideal gaseous mixtures.
Keywords: Xe excimers, infrared cathodoluminescence, density-induced redshift, Collision broadening, dense gas mixtures
Received: 20 Feb 2025; Accepted: 16 Apr 2025.
Copyright: © 2025 Borghesani, Carugno and Chiossi. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
* Correspondence: Armando Francesco Borghesani, Department of Physics and Astronomy, School of Sciences, University of Padua, Padua, 35131, Veneto, Italy
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