{"paper":{"title":"Tracing the Quenching History in Galaxy Clusters in the EAGLE Simulation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Diego Pallero, D. Olave-Rojas, Facundo A. G\\'omez, Nelson D. Padilla, P. Cerulo, R. Demarco, S. Torres-Flores","submitted_at":"2018-12-20T19:01:54Z","abstract_excerpt":"We use the EAGLE hydrodynamical simulation to trace the quenching history of galaxies in its 10 most massive clusters. We use two criteria to identify moments when galaxies suffer significant changes in their star formation activity: {\\it i)} the instantaneous star formation rate (SFR) strongest drop, $\\Gamma_{\\rm SFR}^{\\rm SD}$, and {\\it ii)} a \"quenching\" criterion based on a minimum threshold for the specific SFR of $\\lesssim$ 10$^{-11}\\rm yr^{-1}$. We find that a large fraction of galaxies ($\\gtrsim 60\\%$) suffer their $\\Gamma_{\\rm SFR}^{\\rm SD}$ outside the cluster's R$_{200}$. This ``pre"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1812.08802","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"}