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titleDiscovery of a Hard X-ray Spectrum from the Mixed Morphology SNR W28 with XMM-Newton
Author(jpn)中村, 良子; 馬場, 彩; 石田, 学; 山崎, 了; 立松, 健一; 郡, 和範
Author(eng)Nakamura, Ryoko; Bamba, Aya; Ishida, Manabu; Yamazaki, Ryo; Tatematsu, Kenichi; Kohri, Kazunori; Puhlhofer, Gerd; Wagner, Stefan J.
Author Affiliation(jpn)宇宙航空研究開発機構宇宙科学研究本部; 宇宙航空研究開発機構宇宙科学研究本部; 宇宙航空研究開発機構宇宙科学研究本部; 広島大学理学部物理学科; 国立天文台; 東北大学大学院理学研究科物理学専攻
Author Affiliation(eng)Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS)(JAXA); Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS)(JAXA); Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS)(JAXA); Department of Physical Science, Hiroshima University; National Astronomical Observatory of Japan; Department of Physics, Tohoku University; Institut fur Astronomie und Astrophysik; Landessternwarte, Universitat Heidelberg
Issue Date2010-02-26
Japan Aerospace Exploration Agency (JAXA)
Publication title宇宙航空研究開発機構特別資料:
JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H
Start page40
End page41
Publication date2010-02-26
AbstractWe report on the discovery of a non-thermal X-ray emission from the supernova remnant (SNR) W28. W28 is a cosmic ray accelerator from which GeV and TeV gamma-ray were detected. We analyzed the northeast part of W28, and found a power-law spectrum with a photon index of 2.4 (2.1-2.8) from an inner region which is probably non-thermal X-ray emission caused by particle acceleration. On the assumption that it is synchrotron X-ray, the cooling time of synchrotron photon is consistent with the age of W28 with a few micro-G magnetic field. On the other hand, we have no significant X-ray flux from one of the TeV gamma-ray emission region. Assuming a power-law spectrum with a photon index of 2.66, the same as in the TeV band, we obtained a 2-10 keV flux upper limit of 2.1 x 10(exp -14) ergs/s sq cm. Low brightness in X-ray and the coincidence of the molecular cloud and TeV gamma-ray emission site suggests that TeV gamma-ray is originated from accelerated protons.
DescriptionMeeting Information: The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan
Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science
Keywordsacceleration of particles - ISM: individual (W28) - ISM: supernova remnants - X-ray: ISM
Document TypeConference Paper
JAXA Category特別資料
Report NoJAXA-SP-09-008E

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