Discovery of very high energy γ-ray emission from the BL Lacertae object H 2356-309 with the HESS Cherenkov telescopes

被引：0

作者：

Aharonian, F. ^{[1
]}

Akhperjanian, A.G. ^{[2
]}

Bazer-Bachi, A.R. ^{[3
]}

Beilicke, M. ^{[4
]}

Benbow, W. ^{[1
]}

Berge, D. ^{[1
]}

Bernlöhr, K. ^{[1
,5
]}

Boisson, C. ^{[6
]}

Bolz, O. ^{[1
]}

Borrel, V. ^{[3
]}

Braun, I. ^{[1
]}

Breitling, F. ^{[5
]}

Brown, A.M. ^{[7
]}

Bühler, R. ^{[1
]}

Busching ^{[8
]}

Carrigan, S. ^{[1
]}

Chadwick, P.M. ^{[7
]}

Chounet, L.-M. ^{[9
]}

Cornils, R. ^{[4
]}

Costamante, L. ^{[1
,22
]}

Degrange, B. ^{[9
]}

Dickinson, H.J. ^{[7
]}

Djannati-Ataï, A. ^{[10
,11
]}

Drury, L.O'C. ^{[12
]}

Dubus, G. ^{[9
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[13
]}

Espigat, P. ^{[10
,11
]}

Feinstein, F. ^{[14
]}

Ferrero, E. ^{[13
]}

Fontaine, G. ^{[9
]}

Funk, Seb ^{[5
]}

Funk, S. ^{[1
]}

Gallant, Y.A. ^{[14
]}

Giebels, B. ^{[9
]}

Glicenstein, J.F. ^{[15
]}

Goret, P. ^{[15
]}

Hadjichristidis, C. ^{[7
]}

Hauser, D. ^{[1
]}

Hauser, M. ^{[13
]}

Heinzelmann, G. ^{[4
]}

Henri, G. ^{[16
]}

Hermann, G. ^{[1
]}

Hinton, J.A. ^{[1
,13
]}

Hofmann, W. ^{[1
]}

Holleran, M. ^{[8
]}

Horns, D. ^{[17
]}

Jacholkowska, A. ^{[14
]}

De Jager, O.C. ^{[8
]}

Khélifi, B. ^{[1
,9
]}

机构：

[1] Max-Planck-Institut für Kernphysik, Heidelberg, Germany

[2] Yerevan Physics Institute, Yerevan, Armenia

[3] Centre d'Étude Spatiale des Rayonnements, CNRS, UPS, Toulouse, France

[4] Universität Hamburg, Institut für Experimentalphysik, Hamburg, Germany

[5] Institut für Physik, Humboldt-Universität zu Berlin, Germany

[6] LUTH, UMR 8102 du CNRS, Section de Meudon, France

[7] University of Durham, Department of Physics, Durham, United Kingdom

[8] Unit for Space Physics, North-West University, Potchefstroom, South Africa

[9] Laboratoire Leprince-Ringuet, IN2P3/CNRS, École Polytechnique, Palaiseau, France

[10] APC, Paris, France

[11] UMR 7164, CNRS, Observatoire de Paris

[12] Dublin Institute for Advanced Studies, Ireland

[13] Landessternwarte, Universität Heidelberg, Germany

[14] Laboratoire de Physique Théorique et Astroparticules, IN2P3/CNRS, Université Montpellier II, CC 70, France

[15] DAPNIA/DSM/CEA, CE Saclay, France

[16] Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, France

[17] Institut für Astronomie und Astrophysik, Universität Tübingen, Germany

[18] Laboratoire de Physique Nucléaire et de Hautes Énergies, IN2P3/CNRS, Universités Paris VI and VII, France

[19] Institute of Particle and Nuclear Physics, Charles University, Prague, Czech Republic

[20] Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, Germany

[21] University of Namibia, Windhoek, Namibia

[22] European Associated Laboratory for Gamma-Ray Astronomy

[23] DESY, Platanenallee 6, 15738 Zeuthen, Germany

来源：

Astronomy and Astrophysics | 2006年 / 455卷 / 02期

关键词：

The extreme synchrotron BL Lac object H 2356-309; located at a redshift of z = 0.165; was observed from June to December 2004 with a total exposure of 40 h live-time with the HESS (High Energy Stereoscopic System) array of atmospheric-Cherenkov telescopes (ACTs). Analysis of this data set yields; for the first time; a strong excess of 453 γ-rays (10 standard deviations above background) from H 2356-309; corresponding to an observed integral flux above 200 GeV of I(>200 GeV) = (4.1 ±0.5) × 10-12 cm-2 s-1 (statistical error only). The differential energy spectrum of the source between 200 GeV and 1.3TeV is well-described by a power law with a normalisation (at 1 TeV) of N0 = (3.00 ±0.80 stat ± 0.31sys)× 10-13 cm -2 s-1TeV-1 and a photon index of Γ = 3.09 ± 0.24stat ± 0.10sys. H 2356-309 is one of the most distant BL Lac objects detected at very-high-energy γ-rays so far. Results from simultaneous observations from ROTSE-III (optical); RXTE (X-rays) and NRT (radio) are also included and used together with the HESS data to constrain a single-zone homogeneous synchrotron self-Compton (SSC) model. This model provides an adequate fit to the HESS data when using a reasonable set of model parameters. © ESO 2006;

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页码：461 / 466

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