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          Institute: MPI für Kernphysik     Collection: High-Energy Astrophysics     Display Documents

ID: 276590.0, MPI für Kernphysik / High-Energy Astrophysics
TeV gamma-ray observations of SS-433 and a survey of the surrounding field with the HEGRA IACT-System
Authors:Aharonian, Felix; Akhperjanian, A.; Beilicke, M.; Bernlöhr, K.; Börst, H.-G.; Bojahr, H.; Bolz, O.; Coarasa, T.; Contreras, J.; Cortina, J.; Denninghoff, S.; Fonseca, V.; Girma, M.; Götting, N.; Heinzelmann, G.; Hermann, G.; Heusler, A.; Hofmann, W.; Horns, D.; Jung, I.; Kankanyan, R.; Kestel, M.; Kohnle, A.; Konopelko, A.; Kranich, D.; Lampeiti, H.; Lopez, M.; Lorenz, E.; Lucarelli, F.; Mang, O.; Mazin, D.; Meyer, H.; Mirzoyan, R.; Moralejo, A.; Oña-Wilhelmi, E.; Panter, M.; Plyasheshnikov, A.; Pühlhofer, G.; de los Reyes, R.; Rhode, W.; Ripken, J.; Rowell, Gavin; Sahakian, V.; Samorski, M.; Schilling, M.; Siems, M.; Sobzynska, D.; Stamm, W.; Tluczykont, M.; Vitale, V.; Völk, Heinrich; Wiedner, C.A.; Wittek, W.
Research Context:HEGRA, gamma rays: observations -- stars: individual: SS-433
Date of Publication (YYYY-MM-DD):2005-08-04
Title of Journal:Astronomy & Astrophysics
Journal Abbrev.:A&A
Issue / Number:2
Start Page:635
End Page:643
Copyright:ESO 2005
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present results of a search for TeV -ray emission from the microquasar SS-433 and the surrounding region covering a ~ 8°x8° field of view. Analysis of data taken with the HEGRA stereoscopic system of imaging atmospheric Cerenkov imaging telescopes reveals no evidence of steady or variable emission from any position. Observation times of over 100 h have been achieved in central parts of the field of view. We set 99% confidence level upper limits to a number of a-priori-chosen objects of interest, including SS-443 and its interaction regions, 32 pulsars, 3 supernova remnants and the GeV source GeV J1907+0537. Our upper limit of 3.2% Crab flux (for energies E>0.8 TeV) for the eastern-lobe region e3 of SS-433 permits, after comparison with X-ray fluxes, a lower limit of G on the post-shocked magnetic field in this region. An ensemble upper limit at 0.3% Crab flux (E>0.7 TeV) from a subset (11) of the 32 pulsars implies a maximum of 4.5% of the spin-down pulsar power is available for TeV -ray production. For one of the SNR in our FoV, 3C 396, recent Chandra observations suggest that a central pulsar-driven wind nebula may be the source of X-ray emission. Our upper limit implies that a maximum of 0.1% of the spin-down power from the central source of 3C 396 would be available for TeV -rays.
Free Keywords:HEGRA
gamma rays: observations -- stars: individual: SS-433
External Publication Status:published
Document Type:Article
Affiliations:MPI für Kernphysik/Group of H. J. Völk/High Energy Astrophysics (F. Aharonian)
MPI für Kernphysik/Group of W. Hofmann/Experimental High-Energy Astrophysics (M. Panter, G. Hermann)
MPI für Physik/Abteilung Experimentalphysik
External Affiliations:Yerevan Physics Institute, Alikhanian Br.2, 375036 Yerevan, Armenia
Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany
Universität Kiel, Inst. f. Experimentelle und Angewandte Physik, Leibnizstr. 15-19, 24118 Kiel, Germany
Universität Wuppertal, Fachbereich Physik, Gaußstr. 20, 42097 Wuppertal, Germany
Universität Complutense, Facultad de Ciencias Fisicas, Ciudad Universitaria, 28040 Madrid, Spain
Washington University, St. Louis MO 63130, USA
Humboldt Universität f. Phyik, Unter den Linden 6, 10099 Berlin, Germany
Altai State University, Dimitrov Street 66, 656099 Barnaul, Russia
Landessternwarte Heidelberg, Königstuhl, 69117 Heidelberg, Germany
University Lodz, Poland
Laboratoire Leprince-Ringuet, Ecole Polytechnique, 91128 Palaiseau, France (IN2P3/CNRS)
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