{"paper":{"title":"On the Transition of the Galaxy Quenching Mode at 0.5<z<1 in CANDELS","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Anton M. Koekemoer, Avishai Dekel, Dale Kocevski, Darren Croton, David C. Koo, Dongfei Jiang, Eric F. Bell, F. S. Liu, Guillermo Barro, Hassen M. Yesuf, Jerome J. Fang, Lu Liu, Meng Jia, M. Huertas-Company, Nimish P. Hathi, Pablo G. P\\'erez-Gonz\\'alez, S. M. Faber, Weichen Wang, Wei Tong, Xianmin Meng, Xianzhong Zheng, Yicheng Guo","submitted_at":"2018-05-02T01:37:18Z","abstract_excerpt":"We investigate the galaxy quenching process at intermediate redshift using a sample of $\\sim4400$ galaxies with $M_{\\ast} > 10^{9}M_{\\odot}$ between redshift 0.5 and 1.0 in all five CANDELS fields. We divide this sample, using the integrated specific star formation rate (sSFR), into four sub-groups: star-forming galaxies (SFGs) above and below the ridge of the star-forming main sequence (SFMS), transition galaxies and quiescent galaxies. We study their $UVI$ ($U-V$ versus $V-I$) color gradients to infer their sSFR gradients out to twice effective radii. We show that on average both star-formin"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.00595","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}