@inproceedings{oai:jaxa.repo.nii.ac.jp:00005066,
 author = {松下, 恭子 and 深沢, 泰司 and 林, 克洋 and 小波, さおり and 薙野, 綾 and 大橋, 隆哉 and 佐藤, 浩介 and 田原, 譲 and Matsushita, Kyoko and Fukazawa, Yasushi and Hayashi, Katsuhiro and Konami, Saori and Nagino, Ryo and Ohashi, Takaya and Sato, Kosuke and Tawara, Yuzuru},
 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, With Suzaku, we derived O, Mg, S, Si and Fe abundances of hot intracluster medium (ICM) in clusters of galaxies, and groups of galaxies, and hot interstellar medium (ISM) in elliptical, S0, and spiral galaxies. Especially for regions of low surface brightness, the XIS provides better sensitivity to faint lines of O and Mg, which are predominantly synthesized by supernovae (SN) II. The derived abundance ratios, O/Fe, Mg/Fe, Si/Fe and S/Fe of the ICM, scatter around unity, i.e., the solar ratio, adopting the new solar abundances defined by Lodders (2003). Observed clusters and groups of galaxies with a bright central galaxy show similar Fe abundances of about 0.5 solar at 0.1 - 0.2r(sub 180). In contrast, the metal-mass-to-light ratios for clusters of galaxies tend to be higher than those in groups of galaxies. If metal enrichment occurred before the cluster or group formations, the poor systems would carry relatively smaller metal mass with smaller gas mass, while metal abundance would be similar. The derived Fe abundances of the ISM in elliptical galaxies are about 0.5 - 1.0 solar, indicating a low rate of present metal supply into the ICM. To account for Fe mass in the ICM, the past average rate of SNe Ia was much larger. The derived O and Mg abundances of the ISM in these galaxies are consistent with stellar metallicity which reflects formation histories of these galaxies. Observed low O/Fe ratio of the ISM in a S0 galaxy, NGC 4382, indicates different formation histories between this S0 galaxy and elliptical galaxies. The abundance pattern of the hot ISM in spiral galaxies may depend on their starburst activities., 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: AA0064574134, レポート番号: JAXA-SP-09-008E},
 pages = {344--347},
 publisher = {宇宙航空研究開発機構, Japan Aerospace Exploration Agency (JAXA)},
 title = {Metal enrichment histories from galaxies to clusters},
 volume = {JAXA-SP-09-008E},
 year = {2010}
}