Variations of the TeV energy spectrum at different flux levels of Mkn 421 observed with the HEGRA system of Cherenkov telescopes

By H. C. Aharonian, et al. 2002

127 citations recorded by the source corpus.

F. Aharonian, A. Akhperjanian, M. Beilicke, K. Bernlohr, H. Borst, H. Bojahr, O. Bolz, T. Coarasa, J. Contreras, J. Cortina, L. Costamante, S. Denninghoff, V. Fonseca, M. Girma, N. Gotting, G. Heinzelmann, G. Hermann, A. Heusler, W. Hofmann, D. Horns, I. Jung, R. Kankanyan, M. Kestel, J. Kettler, A. Kohnle, A. Konopelko, H. Kornmeyer, D. Kranich, H. Krawczynski, H. Lampeitl, M. Lopez, E. Lorenz, F. Lucarelli, O. Mang, H. Meyer, R. Mirzoyan, M. Milite, A. Moralejo, E. Ona, M. Panter, A. Plyasheshnikov, G. Puhlhofer, G. Rauterberg, R. Reyes, W. Rhode, J. Ripken, G. Rowell, V. Sahakian, M. Samorski, M. Schilling, M. Siems, D. Sobzynska, W. Stamm, M. Tluczykont, H.J. Volk, C. A. Wiedner, W. Wittek and R. A. Remillard

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7715ce93cb057a8a1a4bc1e813782c58bd019ea9

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In Nuclear and High Energy Physics

Citations in the corpus

Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, background): “15 that the observed energy cutoff of low-redshift blazars (Mkn 501, Aharonian et al. 1999; Mkn 421, Aharonian et al. 2002; and BL Lac 1ES 1959+650, Aharonian et al. 2003) is compatible with this relation.”
Quantum-Spacetime Phenomenology (2008, background): “031) observations of photons of energy up to 45 TeV has been reported [438], although a more robust signal is seen once again up to the 20-TeV range [355, 17].”
New limits on the density of the extragalactic background light in the optical to the far-infrared from the spectra of all known TeV blazars (2007, background): “The measured spectrum of the TeV blazar H 1426+428 at a redshift ofz = 0.129 (Aharonian et al. 2002b) led to a first tentative detection ofan imprint of the EBL in a VHE spectrum (Aharonian et al. 2002b, 2003c).”
An Exceptional Very High Energy Gamma-Ray Flare of PKS 2155–304 (2007, background): “The small difference is surprising since a change of the spectral shape with varying flux levels, typically hardening with increased flux, has often been observed from blazars at X-ray energies (see, e.g., Giommi et al. 1990), as well as in the VHE domain (see, e.g., Aharonian et al. 2002).”
The Crab Nebula and Pulsar between 500 GeV and 80 TeV: Observations with the HEGRA Stereoscopic Air Cerenkov Telescopes (2004, methodology): “The feasibility of survey-type observations is demonstrated by the first serendipitous discovery of an unidentified object with this instrument, named TeV J2035+4130 (Aharonian et al. 2002a).”
THE EXTRAGALACTIC BACKGROUND LIGHT, THE HUBBLE CONSTANT, AND ANOMALIES: CONCLUSIONS FROM 20 YEARS OF TeV GAMMA-RAY OBSERVATIONS (2015, background): “The other fifteen spectra, modeled by LP and EPWL models, correspond either to intensive campaigns in low states of prominent sources (2004-05 MAGIC campaign of Markarian 421, large-zenith-angle H.E.S.S. observations of Markarian 421, 2007 VERITAS campaign on 1ES 2344+514, 2007–2010 campaign of ARGO”
A Multiwavelength View of the TeV Blazar Markarian 421: Correlated Variability, Flaring, and Spectral Evolution (2005, background): “Similar spectral hardening has also been seen at TeVenergies (Krennrich et al. 2002; Aharonian et al. 2002).”
Implications of cosmological gamma-ray absorption - II. Modification of gamma-ray spectra (2003, methodology): “The statistics of the signal are poor, probably resulting from absorption much stronger at four times the distance than for the other blazars (Aharonian et al. 2002, Petry et al. 2002, Costamante et al 2003).”
Synchrotron Self-Compton Analysis of TeV X-Ray-Selected BL Lacertae Objects (2008, methodology): “The campaign of March 2001 was one of the longest and most complete (Fossati et al. 2008), in which it was observed by RXTE, Whipple, HEGRA, and the Mt. Hopkins 48′′ telescope nearly continuously for seven days.”
Is the Giant Radio Galaxy M 87 a TeV Gamma-Ray Emitter? (2003, methodology): “Recently, the BL Lac type objects 1ES 1959+650 (z = 0.047) (Nishiyama et al. 1999; Aharonian et al. 2003b) and the much more distant H 1426+428 (z = 0.129) (Horan et al. 2002; Aharonian et al. 2002a) have also been established as TeV γ-ray emitters.”