@inproceedings{oai:jaxa.repo.nii.ac.jp:00003103,
 author = {鳥羽, 儀樹 and 長尾, 透 and Wang, Wei-Hao and 松原, 英雄 and 秋山, 正幸 and 後藤, 友嗣 and 小山, 佑世 and 大山, 陽一 and 山村, 一誠 and Toba, Yoshiki and Nagao, Toru and Wang, Wei-Hao and Matsuhara, Hideo and Akiyama, Masayuki and Goto, Tomotsugu and Koyama, Yusei and Oyama, Yoichi and Yamamura, Issei},
 book = {宇宙航空研究開発機構特別資料, JAXA Special Publication: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life},
 month = {Mar},
 note = {第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We present the relation between stellar mass and star formation rate (SFR) of a sample of infrared (IR)-bright dust-obscured galaxies (DOGs) that are defined by (i - brackets 22 brackets)(sub AB) greater than 7.0 and flux density at 22 micrometers greater than 3.8 mJy. Combining the Sloan Digital Sky Survey (SDSS), TwoMicron All Sky Survey (TWOMASS), Wide-field Infrared Survey Explorer (WISE), Infrared Astronomical Satellite (IRAS), and AKARI catalogs, we selected 7 IR-bright DOG at Z(sub spec) is greater than 0 and less than 1. We estimated their stellar mass and SFR based on a spectral energy distribution fitting technique, and compared them with main sequence of star-forming galaxies at z is greater than 0 and less than 2 and local ULIRGs. As a result, we found that most of IR-bright DOGs lie significantly above the main sequence of star-forming galaxies at similar redshifts. We conclude that the majority of IRAS- and/or AKARI-detected IR-bright DOGs are starburst galaxies., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026029, レポート番号: JAXA-SP-17-009E},
 pages = {181--184},
 publisher = {宇宙航空研究開発機構(JAXA), Japan Aerospace Exploration Agency (JAXA)},
 title = {Where do infrared-bright dust-obscured galaxies lie on the star formation rate-stellar mass plane?},
 volume = {JAXA-SP-17-009E},
 year = {2018}
}