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Title:
Study of Nonthermal Emission from SNR RX J1713.7-3946 with Suzaku
Authors:
Tanaka, Takaaki; Uchiyama, Yasunobu; Aharonian, Felix A.; Takahashi, Tadayuki; Bamba, Aya; Hiraga, Junko S.; Kataoka, Jun; Kishishita, Tetsuichi; Kokubun, Motohide; Mori, Koji; Nakazawa, Kazuhiro; Petre, Robert; Tajima, Hiroyasu; Watanabe, Shin
Affiliation:
AA(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.; Kavli Institute for Particle Astrophysics and Cosmology Stanford Linear Accelerator Center, 2575 Sand Hill Road M/S 29, Menlo Park, CA 94025.), AB(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.), AC(Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland.; Max-Planck-Institut für Kernphysik, PO Box 103980, D 69029 Heidelberg, Germany.), AD(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.; Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan.), AE(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.), AF(Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan.), AG(Department of Physics, Tokyo Institute of Technology, 2-12-1 Ohokayama, Meguro, Tokyo 152-8551, Japan.), AH(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.; Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan.), AI(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.), AJ(Department of Applied Physics, University of Miyazaki, 1-1 Gakuen Kibana-dai Nishi, Miyazaki 889-2192, Japan.), AK(Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan.), AL(X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771.), AM(Kavli Institute for Particle Astrophysics and Cosmology Stanford Linear Accelerator Center, 2575 Sand Hill Road M/S 29, Menlo Park, CA 94025.), AN(Department of High Energy Astrophysics, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.)
Publication:
The Astrophysical Journal, Volume 685, Issue 2, pp. 988-1004. (ApJ Homepage)
Publication Date:
10/2008
Origin:
UCP
ApJ Keywords:
Acceleration of Particles, ISM: individual (RX J1713.7-3946), ISM: Supernova Remnants, X-Rays: ISM
DOI:
10.1086/591020
Bibliographic Code:
2008ApJ...685..988T

Abstract

We present results obtained from a series of observations of the supernova remnant RX J1713.7-3946 by Suzaku. Hard X-rays have been detected up to ~40 keV. The hard X-ray spectra are described by a power law with photon indices of ~3.0, which is larger than those below 10 keV. The combination of the spatially integrated XIS and HXD spectra clearly reveals a spectral cutoff which is linked to the maximum energy of accelerated electrons. The broadband coverage of Suzaku allows us to derive, for the first time, the energy spectrum of parent electrons in the cutoff region. The cutoff energy in the X-ray spectrum indicates that the electron acceleration in the remnant proceeds close to the Bohm diffusion limit. We discuss the implications of the spectral and morphological properties of the Suzaku data in the context of the origin of nonthermal emission. The Suzaku X-ray and H.E.S.S. gamma-ray data together hardly can be explained within a pure leptonic scenario. Moreover, the leptonic models require a weak magnetic field, which is inconsistent with the recently discovered X-ray filamentary structures and their short-term variability. The hadronic models with strong magnetic fields provide reasonable fits to the observed spectra, but require special arrangements of parameters to explain the lack of thermal X-ray emission. For morphology studies, we compare the X-ray and TeV gamma-ray surface brightness. We confirm the previously reported strong correlation between X-rays and TeV gamma rays. At the same time, the Suzaku data reveal a deviation from the general tendency, namely, the X-ray emission in the western rims appears brighter than expected from the average X-ray to gamma-ray ratio.
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