{"paper":{"title":"Understanding the strong intervening OVI absorber at z$_{abs}$ ~0.93 towards PG1206+459","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Bart P. Wakker, Benjamin E. Rosenwasser, Christopher W. Churchill, Glenn G. Kacprzak, Jane C. Charlton, Sowgat Muzahid","submitted_at":"2018-01-31T19:20:35Z","abstract_excerpt":"We have obtained new observations of the partial Lyman limit absorber at \\zabs$=0.93$ towards quasar PG~1206+459, and revisit its chemical and physical conditions. The absorber, with $ N(HI) \\sim 10^{17.0}$ ~\\sqcm\\ and absorption lines spread over $\\gtrsim$1000~\\kms\\ in velocity, is one of the strongest known OVI absorbers at $\\log N(OVI)=$15.54$\\pm$0.17. Our analysis makes use of the previously known low-(e.g. \\MgII), intermediate-(e.g. SiIV), and high-ionization (e.g., CIV, NV, NeVIII) metal lines along with new $HST/$COS observations that cover OVI, and an $HST/$ACS image of the quasar fiel"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.00026","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"}