Timing analysis techniques at large core distances for multi-TeV gamma ray astronomy

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dc.contributor.authorStamatescu, V.
dc.contributor.authorRowell, G.
dc.contributor.authorDenman, J.
dc.contributor.authorClay, R.
dc.contributor.authorDawson, B.
dc.contributor.authorSmith, A.
dc.contributor.authorSudholz, T.
dc.contributor.authorThornton, G.
dc.contributor.authorWild, N.
dc.date.issued2011
dc.description.abstractWe present an analysis technique that uses the timing information of Cherenkov images from extensive air showers (EAS). Our emphasis is on distant, or large core distance γ-ray induced showers at multi-TeV energies. Specifically, combining pixel timing information with an improved direction reconstruction algorithm, leads to improvements in angular and core resolution as large as ∼40% and ∼30%, respectively, when compared with the same algorithm without the use of timing. Above 10 TeV, this results in an angular resolution approaching 0.05°, together with a core resolution better than ∼15 m. The off-axis post-cut γ-ray acceptance is energy dependent and its full width at half maximum ranges from 4° to 8°. For shower directions that are up to ∼6° off-axis, the angular resolution achieved by using timing information is comparable, around 100 TeV, to the on-axis angular resolution. The telescope specifications and layout we describe here are geared towards energies above 10 TeV. However, the methods can in principle be applied to other energies, given suitable telescope parameters. The 5-telescope cell investigated in this study could initially pave the way for a larger array of sparsely spaced telescopes in an effort to push the collection area to >10 km<sup>2</sup>. These results highlight the potential of a 'sparse array' approach in effectively opening up the energy range above 10 TeV. © 2011 Elsevier B.V. All rights reserved.
dc.description.statementofresponsibilityV. Stamatescu, G.P. Rowell, J. Denman, R.W. Clay, B.R. Dawson, A.G.K. Smith, T. Sudholz, G.J. Thornton and N. Wild
dc.description.urihttp://www.elsevier.com/wps/find/journaldescription.cws_home/523319/description#description
dc.identifier.citationAstroparticle Physics, 2011; 34(12):886-896
dc.identifier.doi10.1016/j.astropartphys.2011.03.008
dc.identifier.issn0927-6505
dc.identifier.issn1873-2852
dc.identifier.orcidRowell, G. [0000-0002-9516-1581]
dc.identifier.orcidClay, R. [0000-0002-9040-9648]
dc.identifier.orcidDawson, B. [0000-0002-4271-3055]
dc.identifier.urihttp://hdl.handle.net/2440/66842
dc.language.isoen
dc.publisherElsevier Science BV
dc.relation.granthttp://purl.org/au-research/grants/arc/DP0662810
dc.relation.granthttp://purl.org/au-research/grants/arc/DP0662810
dc.rightsCopyright 2011 Elsevier B.V. All rights reserved.
dc.source.urihttps://doi.org/10.1016/j.astropartphys.2011.03.008
dc.subjectGamma-ray astronomy
dc.subjectCosmic rays
dc.subjectImaging atmospheric Cherenkov telescopes
dc.subjectInstrumentation
dc.titleTiming analysis techniques at large core distances for multi-TeV gamma ray astronomy
dc.typeJournal article
pubs.publication-statusPublished

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