{"paper":{"title":"Galaxy And Mass Assembly (GAMA): The sSFR-M* relation part I - $\\sigma_{\\mathrm{sSFR}}$-M* as a function of sample, SFR indicator and environment","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Katsianis, A. S. G. Robotham, B. W. Holwerda, C. del P. Lagos, L. Cortese, L. J. M. Davies, M. E. Cluver, M. J. I. Brown, M. N. Bremer, M. Owers, M.W. Grootes, S. Brough, S. P. Driver, S. Phillipps","submitted_at":"2018-11-08T23:14:48Z","abstract_excerpt":"Recently a number of studies have proposed that the dispersion along the star formation rate - stellar mass relation ($\\sigma_{\\mathrm{sSFR}}$-M$_{*}$) is indicative of variations in star-formation history (SFH) driven by feedback processes. They found a 'U'-shaped dispersion and attribute the increased scatter at low and high stellar masses to stellar and active galactic nuclei feed-back respectively. However, measuring $\\sigma_{\\mathrm{sSFR}}$ and the shape of the $\\sigma_{\\mathrm{sSFR}}$-M$_{*}$ relation is problematic and can vary dramatically depending on the sample selected, chosen separ"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1811.03712","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"}