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The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, The X-ray Imaging Spectrometer (XIS) onboard Suzaku is characterized by three major advantages: low and stable background, good response in low energies, and superior energy resolution. Utilizing these advantages, the XIS has attacked a number of supernova remnants (SNRs). The first advantageous point allows us to detect Fe, Mn, and Cr lines from young SNRs, while the second one reveals C and N lines from evolved SNRs. The third one enables us to detect line broadening due to either the Doppler effect, the thermal Doppler effect, or the ionization-timescale variation of several plasma components. For largely extended evolved SNRs, by combining the three advantages, spatially-resolved spectral analyses show us their metal distributions in unprecedented details. I will review such a Suzaku view of thermal SNRs, 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: AA0064574023, レポート番号: JAXA-SP-09-008E

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 performed a comprehensive study of the Cygnus Loop, which is one of the largest (R approximately 80 min) and the brightest supernova remnants (SNRs) in the X-ray sky. In spite that it is a middle-aged SNR (approximately 10,000 yr), there is a substantial amount of fresh metal ejected from the progenitor. We have been observing this SNR since 2002 with Suzaku and XMM-Newton observatories, and now we have 41 pointing observation data sets in total. Here we report the results of our observations., 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: AA0064574013, レポート番号: JAXA-SP-09-008E

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, SXI (Soft X-ray Imager) is the X-ray CCD camera system consisting of 4 back-illuminated CCD chips of 1280 x 1280 - pixel format, each of which is read out with 2 x 2 on-chip binning scheme at every 4 sec, and a couple of single stage Stirling coolers. The incident optical photons are blocked by OBL (optical blocking layer) coated on the chips instead of traditional optical blocking filters. The contamination on OBL from the spacecraft is controlled by a baffle connecting the camera body and the X-ray telescope mirror. The CCD driver and ADC are placed in the camera body unit, and no analog signal appears among the SXI components. All the analog and digital BBMs have already been built, while some functions in the digital part have not implemented yet and the end-to-end analog performance has not investigated yet., 著者人数: 22人(含チーム1), Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, Number of authors: 22, 資料番号: AA0064574177, レポート番号: JAXA-SP-09-008E

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