{"paper":{"title":"Chandra observations of the galaxy group AWM 5: cool core re-heating and thermal conduction suppression","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) Max Planck Institute for Extraterrestrial Physics), A. Baldi (1), A. Simionescu (2) ((1) Harvard-Smithsonian Center for Astrophysics, C. Jones (1), L. David (1), P. Nulsen (1), R. Kraft (1), W. Forman (1)","submitted_at":"2008-11-22T01:29:16Z","abstract_excerpt":"We present an analysis of a 40 ksec Chandra observation of the galaxy group AWM 5. It has a small ($\\sim8$ kpc) dense cool core with a temperature of $\\sim1.2$ keV and the temperature profile decreases at larger radii, from $\\sim3.5$ keV just outside the core to $\\sim2$ keV at $\\sim300$ kpc from the center. The abundance distribution shows a \"hole\" in the central $\\sim10$ kpc, where the temperature declines sharply. An abundance of at least a few times solar is observed $\\sim15-20$ kpc from the center. The deprojected electron density profile shows a break in slope at $\\sim13$ kpc and can be f"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0811.3654","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"}