@inproceedings{oai:jaxa.repo.nii.ac.jp:00020311, author = {諸田, 智克 and 春山, 純一 and 大竹, 真紀子 and 松永, 恒雄 and 本田, 親寿 and 横田, 康弘 and 木村, 淳 and 小川, 佳子 and 平田, 成 and 出村, 裕英 and 岩崎, 晃 and 杉原, 孝充 and 佐伯, 和人 and 中村, 良介 and 小林, 進悟 and Morota, Tomokatsu and Haruyama, Junichi and Otake, Makiko and Matsunaga, Tsuneo and Honda, Chikatoshi and Yokota, Yasuhiro and Kimura, Jun and Ogawa, Yoshiko and Hirata, Naru and Demura, Hirohide and Iwasaki, Akira and Sugihara, Takamitsu and Saiki, Kazuto and Nakamura, Ryosuke and Kobayashi, Shingo}, book = {第43回月・惑星シンポジウム, Proceedings of the 43th ISAS Lunar and Planetary Symposium}, month = {Aug}, note = {第43回月・惑星シンポジウム (2010年8月4-6日. 宇宙航空研究開発機構宇宙科学研究所), 相模原市, 神奈川県, 43rd ISAS Lunar and Planetary Symposium (August 4-6, 2010. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, Unraveling the timing and duration of mare volcanism on the Moon is essential for understanding its thermal evolution. The end of mare volcanism is poorly constrained, because mare basalts are incompletely sampled. In this study, employing SELENE (Kaguya) high-resolution images, we performed new crater size-frequency measurements for 49 young mare units (