@inproceedings{oai:jaxa.repo.nii.ac.jp:00004978,
 author = {小杉, 寛子 and 常深, 博 and 内田, 裕之 and 木村, 公 and 勝田, 哲 and Kosugi, Hiroko and Tsunemi, Hiroshi and Uchida, Hiroyuki and Kimura, Masashi and Katsuda, Satoru},
 book = {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},
 month = {Feb},
 note = {The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We observed the south-east (SE) limb (P26, P27, and P28) of the Cygnus Loop supernova remnant(SNR) with Suzaku. The X-ray morphologies of P26 and P28 show concaved structures relative to the other shell regions of the Loop. Levenson et al. (2005) insisted that the concave seen in P26 is due to the interaction of the supernova blast wave with a large scale interstellar cloud from their Chandra observation. We perform spatially resolved spectroscopy for the Suzaku data. Applying a single temperature NEI model, we generate maps of the electron temperature, the ionization time scale, the emission measure, and metal abundances. Based on the maps, we propose that the blast wave is hitting interstellar clouds in P28 as well as P26, while the blast wave is propagating into a relatively uniform ambient medium in P26., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574046, レポート番号: JAXA-SP-09-008E},
 pages = {120--121},
 publisher = {宇宙航空研究開発機構, Japan Aerospace Exploration Agency (JAXA)},
 title = {Suzaku Observation of the South-East Limb of the Cygnus Loop},
 volume = {JAXA-SP-09-008E},
 year = {2010}
}