{"paper":{"title":"The MUSE Hubble Ultra Deep Field Survey XI. Constraining the low-mass end of the stellar mass - star formation rate relation at $z<1$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Corentin Schreiber, Hanae Inami, Jarle Brinchmann, Johannes Zabl, Johan Richard, Joop Schaye, Leindert A. Boogaard, Lutz Wisotzki, Madusha L. P. Gunawardhana, Michael V. Maseda, Mieke Paalvast, Nicolas Bouch\\'e, Peter Mitchell, Raffaella A. Marino, Roland Bacon, Rychard J. Bouwens, Sandro Tacchella, Themiya Nanayakkara, Thierry Contini","submitted_at":"2018-08-14T21:26:19Z","abstract_excerpt":"Star-forming galaxies have been found to follow a relatively tight relation between stellar mass ($M_{*}$) and star formation rate (SFR), dubbed the `star formation sequence'. A turnover in the sequence has been observed, where galaxies with $M_{*} < 10^{10} {\\rm M}_{\\odot}$ follow a steeper relation than their higher mass counterparts, suggesting that the low-mass slope is (nearly) linear. In this paper, we characterise the properties of the low-mass end of the star formation sequence between $7 \\leq \\log M_{*}[{\\rm M}_{\\odot}] \\leq 10.5$ at redshift $0.11 < z < 0.91$. We use the deepest MUSE"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1808.04900","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"}