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

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dc.creatorSchroedter, M.
dc.creatorBadran, H. M.
dc.creatorBuckley, J. H.
dc.creatorGordo, J. Bussons
dc.creatorCarter-Lewis, D. A.
dc.creatorDuke, C.
dc.creatorFegan, D. J.
dc.creatorFegan, S. F.
dc.creatorFinley, J. P.
dc.creatorGillanders, G. H.
dc.creatorGrube, J.
dc.creatorHoran, D.
dc.creatorKenny, G. E.
dc.creatorKertzman, M.
dc.creatorKosack, K.
dc.creatorKrennrich, F.
dc.creatorKieda, D. B.
dc.creatorKildea, J.
dc.creatorLang, M. J.
dc.creatorLee, Kuen
dc.creatorMoriarty, P.
dc.creatorQuinn, J.
dc.creatorQuinn, M.
dc.creatorPower-Mooney, G. B.
dc.creatorSembroski, H.
dc.creatorWakely, S. P.
dc.creatorVassiliev, V. V.
dc.creatorWeekes, T. C.
dc.creatorZweerink, J.
dc.date2005-08-23
dc.date.accessioned2026-07-07T10:43:18Z
dc.date.available2026-07-07T10:43:18Z
dc.descriptionThe 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.description27 pages, 11 figures, accepted by ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0508499
dc.identifierhttp://arxiv.org/abs/astro-ph/0508499
dc.identifierAstrophys.J.634:947-954,2005
dc.identifierdoi:10.1086/496968
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/182192
dc.subjectAstrophysics
dc.titleA Very High Energy Gamma-Ray Spectrum of 1ES 2344+514
dc.typetext

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