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Very high energy gamma-quanta 1–65 TeV from the Cygnus X-3 binary

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Title: Very high energy gamma-quanta 1–65 TeV from the Cygnus X-3 binary
Authors: Sinitsyna, V.G.1, Arsov, T.P.1, Alaverdian, A.Y.1, Borisov, S.S.1, Musin, F.I.1, Mirzafatikov, R.M.1, Nikolsky, S.I.1, Sinitsyna, V.Y.1, Platonov, G.F.1, Capdevielle, J.-N.2
Source: Nuclear Physics B Proceedings Supplement. Feb2006, Vol. 151 Issue 1, p489-492. 4p.
Subjects: Gamma rays, Telescopes, Detectors, Astronomical instruments
Abstract: The results of almost ten-year observation of Cygnus X-3 point source by SHALON mirror Cherenkov telescope are presented. The galactic source Cygnus X-3, known for more than 10 years as a source with variable intensity , was regularly observed since 1995 with average gamma-quantum flux . The flux in 2003 was . Earlier, in 1997, an increase in the flux was also observed . The limits on gamma-rays from Cygnus X-3, the source that results stimulated the construction of many new detectors are presented. These upper limits and SHALON fluxes are now more than a factor 100 less than the fluxes originally reported. [Copyright &y& Elsevier]
Copyright of Nuclear Physics B Proceedings Supplement is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Engineering Source
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Header DbId: egs
DbLabel: Engineering Source
An: 19139455
AccessLevel: 6
PubType: Periodical
PubTypeId: serialPeriodical
PreciseRelevancyScore: 0
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  Data: Very high energy gamma-quanta 1–65 TeV from the Cygnus X-3 binary
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  Data: <searchLink fieldCode="AR" term="%22Sinitsyna%2C+V%2EG%2E%22">Sinitsyna, V.G.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Arsov%2C+T%2EP%2E%22">Arsov, T.P.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Alaverdian%2C+A%2EY%2E%22">Alaverdian, A.Y.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Borisov%2C+S%2ES%2E%22">Borisov, S.S.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Musin%2C+F%2EI%2E%22">Musin, F.I.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Mirzafatikov%2C+R%2EM%2E%22">Mirzafatikov, R.M.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Nikolsky%2C+S%2EI%2E%22">Nikolsky, S.I.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Sinitsyna%2C+V%2EY%2E%22">Sinitsyna, V.Y.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Platonov%2C+G%2EF%2E%22">Platonov, G.F.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Capdevielle%2C+J%2E-N%2E%22">Capdevielle, J.-N.</searchLink><relatesTo>2</relatesTo>
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  Data: <searchLink fieldCode="JN" term="%22Nuclear+Physics+B++Proceedings+Supplement%22">Nuclear Physics B Proceedings Supplement</searchLink>. Feb2006, Vol. 151 Issue 1, p489-492. 4p.
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  Data: The results of almost ten-year observation of Cygnus X-3 point source by SHALON mirror Cherenkov telescope are presented. The galactic source Cygnus X-3, known for more than 10 years as a source with variable intensity , was regularly observed since 1995 with average gamma-quantum flux . The flux in 2003 was . Earlier, in 1997, an increase in the flux was also observed . The limits on gamma-rays from Cygnus X-3, the source that results stimulated the construction of many new detectors are presented. These upper limits and SHALON fluxes are now more than a factor 100 less than the fluxes originally reported. [Copyright &y& Elsevier]
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  Data: <i>Copyright of Nuclear Physics B Proceedings Supplement is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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              Text: Feb2006
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