![]() We observe no significant difference between the γ-ray spectra of the immediate GC surroundings, which we model as a point source (Sgr A*) and the Galactic Ridge. ![]() We obtain a significant detection for all four model components used to fit our data (Sgr A*, “Arc”, G0.9+0.1, and an extended component for the Galactic Ridge). We present a discussion of the associated biases and limitations of such an approach. We used existing measurements of the gas distribution in the GC region to derive the underlying distribution of CRs. Using recently developed software tools, we derived the instrument response and background models required for extracting the diffuse emission in the region. ![]() Those were collected at high zenith angles (58−70 deg), leading to a larger energy threshold, but also an increased effective collection area compared to low zenith observations. We used data from ≈100 h observations of the GC region conducted with the MAGIC telescopes over five years (from 2012 to 2017). Here we present deep observations of the Galactic center (GC) region with the MAGIC telescopes and use them to infer the underlying CR distribution and to study the alleged PeV proton accelerator at the center of our Galaxy. In the presence of a sufficient amount of target material, γ-rays can be used as a tracer in the search for sources of Galactic cosmic rays (CRs). of Physics & Astronomy, University of Bologna, Bologna, ItalyĪims. Port d’Informació Científica (PIC), 08193 Bellaterra, Barcelona, Spainĭipartimento di Fisica, Università di Trieste, 34127 Trieste, Italy Universitat de Barcelona, ICCUB, IEEC-UB, 08028 Barcelona, Spain Energy, Bulgarian Academy of Sciences, 1784 Sofia, Bulgaria Japanese MAGIC Consortium: ICRR, The University of Tokyo, 277-8582 Chiba, Japan Department of Physics, Kyoto University, 606-8502 Kyoto, Japan Tokai University, 259-1292 Kanagawa, Japan RIKEN, 351-0198 Saitama, Japan Universität Würzburg, 97074 Würzburg, Germanyįinnish MAGIC Consortium: Finnish Centre of Astronomy with ESO (FINCA), University of Turku, 20014 Turku, Finland Astronomy Research Unit, University of Oulu, 90014 Oulu, Finlandĭepartament de Física and CERES-IEEC, Universitat Autònoma de Barcelona, 08193 Bellaterra, Spain ICRANet-Armenia at NAS RA, 0019 Yerevan, ArmeniaĬentro de Investigaciones Energéticas, Medioambientales y Tecnológicas, 28040 Madrid, Spain Università di Pisa and INFN Pisa, 56126 Pisa, Italy Università di Padova and INFN, 35131 Padova, Italy Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), 08193 Bellaterra, Barcelona, Spain Max-Planck-Institut für Physik, 80805 München, Germany Istituto Nazionale Fisica Nucleare (INFN), 00044 Frascati, Roma, Italy Università di Siena and INFN Pisa, 53100 Siena, Italyĭeutsches Elektronen-Synchrotron (DESY), 15738 Zeuthen, Germany University of Łódź, Department of Astrophysics, 90236 Łódź, Poland IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, 28040 Madrid, Spain Saha Institute of Nuclear Physics, HBNI, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, IndiaĬentro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro, RJ, Brasil Technische Universität Dortmund, 44221 Dortmund, GermanyĬroatian Consortium: University of Rijeka, Department of Physics, 51000 Rijeka University of Split – FESB, 21000 Split University of Zagreb – FER, 10000 Zagreb University of Osijek, 31000 Osijek Rudjer Boskovic Institute, 10000 Zagreb, Croatia National Institute for Astrophysics (INAF), 00136 Rome, Italy Università di Udine and INFN Trieste, 33100 Udine, Italy Astrofísica, 38206 La Laguna, Tenerife, Spain de Astrofísica de Canarias, 38200 La Laguna, Spain Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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