{"paper":{"title":"XRISM detection of the 6.4 keV Fe K$\\alpha$ line in the radio galaxy Cygnus A","license":"http://creativecommons.org/licenses/by/4.0/","headline":"XRISM Resolve spectrum reveals two Keplerian Fe Kα components in Cygnus A at distances of 0.1-0.17 pc and 6-10 pc from the black hole.","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"Anwesh Majumder, A. Ptak, A. Simionescu, B.R. McNamara, E. Hodges-Kluck, L. Gu, M.W. Wise, M. Yukita, N. Roy, T. Heckman","submitted_at":"2026-05-16T02:36:55Z","abstract_excerpt":"We detail the spectral analysis of a 170 ks XRISM Resolve observation of the core of Cygnus A. The high spectral resolution of Resolve have enabled us to probe the inner accretion region of Cygnus A by analyzing the 6.4 keV Fe K$\\alpha$ line complex. We find that it consists of two Keplerian broadened components. (1) A broad component with a velocity dispersion of $3400^{+800}_{-600}$ km s$^{-1}$ and (2) a narrow component of $440^{+60}_{-50}$ km s$^{-1}$. For an inclination of $50^{\\circ}-85^{\\circ}$, constrained by VLBI, we find that the broad component arises from a distance of $\\sim 0.1-0."},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The broad Fe Kα component arises from a distance of ∼0.1-0.17 pc (800-1400 gravitational radii) and the narrow component from ∼6-10 pc (50,000-80,000 gravitational radii) from the central black hole, for inclinations 50°-85° constrained by VLBI.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The assumption that both line components are purely Keplerian orbits viewed at the VLBI-constrained inclination range of 50°-85°, with no significant contribution from non-gravitational motions or complex geometry that would change the inferred radii (stated in the distance calculation paragraph after the velocity dispersion results).","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"XRISM Resolve spectrum of Cygnus A resolves the Fe Kα line into two Keplerian components at ~0.1 pc (broad) and ~6-10 pc (narrow), consistent with BLR and torus origins.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"XRISM Resolve spectrum reveals two Keplerian Fe Kα components in Cygnus A at distances of 0.1-0.17 pc and 6-10 pc from the black hole.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"770c6bdc863b27403e314ce8ba92d9a59d9c54123bb0be657693f2ade3964058"},"source":{"id":"2605.16766","kind":"arxiv","version":1},"verdict":{"id":"f95084da-8f66-458d-a2cf-aefde0ac1a86","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T20:51:32.347150Z","strongest_claim":"The broad Fe Kα component arises from a distance of ∼0.1-0.17 pc (800-1400 gravitational radii) and the narrow component from ∼6-10 pc (50,000-80,000 gravitational radii) from the central black hole, for inclinations 50°-85° constrained by VLBI.","one_line_summary":"XRISM Resolve spectrum of Cygnus A resolves the Fe Kα line into two Keplerian components at ~0.1 pc (broad) and ~6-10 pc (narrow), consistent with BLR and torus origins.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The assumption that both line components are purely Keplerian orbits viewed at the VLBI-constrained inclination range of 50°-85°, with no significant contribution from non-gravitational motions or complex geometry that would change the inferred radii (stated in the distance calculation paragraph after the velocity dispersion results).","pith_extraction_headline":"XRISM Resolve spectrum reveals two Keplerian Fe Kα components in Cygnus A at distances of 0.1-0.17 pc and 6-10 pc from the black hole."},"integrity":{"clean":false,"summary":{"advisory":0,"critical":1,"by_detector":{"doi_compliance":{"total":1,"advisory":0,"critical":1,"informational":0}},"informational":0},"endpoint":"/pith/2605.16766/integrity.json","findings":[{"note":"Identifier '10.5281/zenodo.19441335' is syntactically valid but the DOI registry (doi.org) returned 404, and Crossref / OpenAlex / internal corpus also have no record. The cited work could not be located through any authoritative source.","detector":"doi_compliance","severity":"critical","ref_index":29,"audited_at":"2026-05-19T21:01:43.135510Z","detected_doi":"10.5281/zenodo.19441335","finding_type":"unresolvable_identifier","verdict_class":"cross_source","detected_arxiv_id":null}],"available":true,"detectors_run":[{"name":"doi_compliance","ran_at":"2026-05-19T21:01:43.135510Z","status":"completed","version":"1.0.0","findings_count":1},{"name":"doi_title_agreement","ran_at":"2026-05-19T21:01:19.273705Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"claim_evidence","ran_at":"2026-05-19T19:01:56.314438Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"ai_meta_artifact","ran_at":"2026-05-19T18:33:26.447833Z","status":"skipped","version":"1.0.0","findings_count":0}],"snapshot_sha256":"b0099dca103ea3a6a9364a3a24558aa2de29fb4f015c73831cd9cc87841ddeac"},"references":{"count":57,"sample":[{"doi":"10.1038/371313a0","year":1994,"title":"1994, Nature, 371, 313, doi: 10.1038/371313a0 Astropy Collaboration, Robitaille, T","work_id":"3854a381-16e8-46d6-a685-d7f8bab1664b","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1086/165571","year":1987,"title":"1987, ApJ, 320, 537, doi: 10.1086/165571","work_id":"3a51ce85-549c-4f1b-a4d7-6ed50ce3202f","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1051/0004-6361/201628412","year":2016,"title":"Zensus, J. A. 2016, Astronomy & Astrophysics, 588, L9, doi: 10.1051/0004-6361/201628412","work_id":"f1e149c1-95cd-4b8a-b284-aa39253d0ff6","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.48550/arxiv.2507.02195","year":2025,"title":"2025, arXiv, doi: 10.48550/arXiv.2507.02195","work_id":"22f9dbb8-a854-4ccd-9d5d-2ab2e1702ae7","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1051/0004-6361/201321890","year":2013,"title":"Burtscher, L., Meisenheimer, K., Tristram, K. R. W., et al. 2013, Astronomy & Astrophysics, 558, A149, doi: 10.1051/0004-6361/201321890","work_id":"a59b0b50-67e8-42af-a712-0a1923b513c5","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":57,"snapshot_sha256":"8c54bcede9eafec8d772eef9080913b0ee3259a4ccac0458a8f12e5a0fce18e6","internal_anchors":0},"formal_canon":{"evidence_count":2,"snapshot_sha256":"9e988a3e59872851f0b783f29420905552f29f9042e6a1815e70a8be6bce7e30"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}