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A Very High Energy Gamma-Ray Spectrum of 1ES 2344+514

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dc.contributor.author Lang, Mark
dc.contributor.author Gillanders, Gary
dc.date.accessioned 2012-01-20T11:33:00Z
dc.date.available 2012-01-20T11:33:00Z
dc.date.issued 2005
dc.identifier.citation M. Schroedter, H. M. Badran, J. H. Buckley, J. Bussons Gordo, D. A. Carter-Lewis, C. Duke, D. J. Fegan, S. F. Fegan, J. P. Finley, G. H. Gillanders, J. Grube, D. Horan, G. E. Kenny, M. Kertzman, K. Kosack, F. Krennrich, D. B. Kieda, J. Kildea, M. J. Lang, Kuen Lee, P. Moriarty, J. Quinn, M. Quinn, G. B. Power-Mooney, H. Sembroski, S. P. Wakely, V. V. Vassiliev, T. C. Weekes, J. Zweerink(2005)A Very High Energy Gamma-Ray Spectrum of 1ES 2344+514, Astrophys.J.634:947-954,2005 en_US
dc.identifier.uri http://hdl.handle.net/10379/2516
dc.description.abstract The BL Lacertae (BL Lac) object 1ES 2344+514 (1ES 2344), at a redshift of 0.044, was discovered as a source of very high energy (VHE) gamma rays by the Whipple Collaboration in 1995 \citep{2344Catanese98}. This detection was recently confirmed by the HEGRA Collaboration \citep{2344Hegra03}. As is typical for high-frequency peaked blazars, the VHE gamma-ray emission is highly variable. On the night of 20 December, 1995, a gamma-ray flare of 5.3-sigma significance was detected, the brightest outburst from this object to-date. The emission region is compatible with a point source. The spectrum between 0.8 TeV and 12.6 TeV can be described by a power law $\frac{\ud^3 N}{\ud E \ud A \ud t}=(5.1\pm1.0_{st}\pm1.2_{sy})\times10^{-7} (E/ \mathrm{TeV})^{-2.54 \pm0.17_{st}\pm0.07_{sy}} \mathrm{\frac{1}{TeV m^2 s}}$. Comparing the spectral index with that of the other five confirmed TeV blazars, the spectrum of 1ES 2344 is similar to 1ES 1959+650, located at almost the same distance. The spectrum of 1ES 2344 is steeper than the brightest flare spectra of Markarian 421 (Mrk~421) and Markarian 501 (Mrk~501), both located at a distance about 2/3 that of 1ES 2344, and harder than the spectra of PKS 2155-304 and H~1426+428, which are located almost three times as far. This trend is consistent with attenuation caused by the infrared extragalactic background radiation.
dc.format application/pdf en_US
dc.language.iso en en_US
dc.subject Astrophysics
dc.title A Very High Energy Gamma-Ray Spectrum of 1ES 2344+514 en_US
dc.type Article en_US
dc.local.publishedsource http://arxiv.org/pdf/astro-ph/0508499 en_US
dc.description.peer-reviewed peer-reviewed en_US
dc.local.authors M. Schroedter, H. M. Badran, J. H. Buckley, J. Bussons Gordo, D. A. Carter-Lewis, C. Duke, D. J. Fegan, S. F. Fegan, J. P. Finley, G. H. Gillanders, J. Grube, D. Horan, G. E. Kenny, M. Kertzman, K. Kosack, F. Krennrich, D. B. Kieda, J. Kildea, M. J. Lang, Kuen Lee, P. Moriarty, J. Quinn, M. Quinn, G. B. Power-Mooney, H. Sembroski, S. P. Wakely, V. V. Vassiliev, T. C. Weekes, J. Zweerink
dc.local.arxivid astro-ph/0508499

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