Study and parametrization of the night sky background radiation spectrum in the range 3000-6000 Å, for use with air fluorescence detectors of UHECR

Moyssides, PG; Maltezos, S; Fokitis, E

dc.contributor.author	Moyssides, PG	en
dc.contributor.author	Maltezos, S	en
dc.contributor.author	Fokitis, E	en
dc.date.accessioned	2014-03-01T01:54:30Z
dc.date.available	2014-03-01T01:54:30Z
dc.date.issued	2005	en
dc.identifier.issn	09500340	en
dc.identifier.uri	https://dspace.lib.ntua.gr/xmlui/handle/123456789/27418
dc.subject.other	Cosmic rays	en
dc.subject.other	Fluorescence	en
dc.subject.other	Nitrogen	en
dc.subject.other	Telescopes	en
dc.subject.other	Fluorescence telescopes	en
dc.subject.other	Optical noise	en
dc.subject.other	Radiation spectrum	en
dc.subject.other	Radiation effects	en
dc.title	Study and parametrization of the night sky background radiation spectrum in the range 3000-6000 Å, for use with air fluorescence detectors of UHECR	en
heal.type	journalArticle	en
heal.identifier.primary	10.1080/09500340410001703869	en
heal.identifier.secondary	http://dx.doi.org/10.1080/09500340410001703869	en
heal.publicationDate	2005	en
heal.abstract	The fluorescence light, induced by showers of the extremely high energy cosmic rays, is produced through the excitation of, mainly, nitrogen molecules, atoms, and ions, in the atmosphere. The fluorescence telescopes of the Auger Project record this nitrogen radiation under the variable night sky optical noise (background radiation) and, therefore, the study of the latter is crucial. In this paper we present a parametrization of an experimental night sky background radiation spectrum that, to our knowledge, is being carried out for the first time, recorded in the range 3000-6000 Å. Although the parametrization described here refers to a particular spectrum, our results are generally applicable, and could be adapted to those prevailing in particular locations, where EAS fluorescence telescopes are operating if, in addition, the gradual time variations of the spectrum are taken into account. They could be useful in data analysis for the event reconstruction, during the operation of the fluorescence detector of the Auger Observatory, since they could be used for the experimental emulation of the optical noise. In addition, they could be used in the designing of air fluorescence observatory components, such as photomultipliers and their spectral sensitivity, as well as in the corresponding optical filters. © 2005 Taylor & Francis Ltd.	en
heal.journalName	Journal of Modern Optics	en
dc.identifier.doi	10.1080/09500340410001703869	en
dc.identifier.volume	52	en
dc.identifier.issue	1	en
dc.identifier.spage	131	en
dc.identifier.epage	146	en