{"paper":{"title":"Calibrating Star Formation in WISE using Total Infrared Luminosity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"D.A. Dale, J.-D.T. Smith, M.E. Cluver, M.J.I. Brown, T. August, T.H. Jarrett","submitted_at":"2017-10-10T09:28:42Z","abstract_excerpt":"We present accurate resolved $WISE$ photometry of galaxies in the combined SINGS and KINGFISH sample. The luminosities in the W3 12$\\mu$m and W4 23$\\mu$m bands are calibrated to star formation rates (SFRs) derived using the total infrared luminosity, avoiding UV/optical uncertainties due to dust extinction corrections. The W3 relation has a 1-$\\sigma$ scatter of 0.15 dex over nearly 5 orders of magnitude in SFR and 12$\\mu$m luminosity, and a range in host stellar mass from dwarf (10$^7$ M$_\\odot$) to $\\sim3\\times$M$_\\star$ (10$^{11.5}$ M$_\\odot$) galaxies. In the absence of deep silicate absor"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.03469","kind":"arxiv","version":2},"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"}