{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:AKMX2EDTAIFK37YEP26P3KHX7U","short_pith_number":"pith:AKMX2EDT","schema_version":"1.0","canonical_sha256":"02997d1073020aadff047ebcfda8f7fd2f91b29aa30de02ee735b366e8f26590","source":{"kind":"arxiv","id":"2604.27061","version":1},"attestation_state":"computed","paper":{"title":"Unveiling the dynamics of the ultra-fast outflow in IRAS 13224-3809 with X-ray spectroscopy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"IRAS 13224-3809 hosts a variable ultra-fast outflow exceeding 0.2c that accelerates rapidly during X-ray flares.","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"Alessia Tortosa, Alfredo Luminari, Enrico Piconcelli, Fabrizio Nicastro, Francesco Tombesi, Giorgio Lanzuisi, Luca Zappacosta, Marco Laurenti, Massimo Gaspari, Pierpaolo Cond\\`o, Riccardo Middei, Roberto Serafinelli","submitted_at":"2026-04-29T18:01:02Z","abstract_excerpt":"IRAS 13224-3809 is one of the most intensively studied narrow-line Seyfert 1 galaxies, with a rich literature reporting diverse and sometimes contrasting interpretations of its complex X-ray spectra and variability. Notably, a fast and variable ultra-fast outflow (UFO) was discovered in this source, sparking debate over its nature and driving mechanisms. Motivated by these open questions, we present a systematic, time- and flux-resolved reanalysis of the full 2016 XMM-Newton (1.5 Ms) and NuSTAR (500 ks) datasets, employing careful background treatment and equal-count spectral selections. We un"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":true,"formal_links_present":false},"canonical_record":{"source":{"id":"2604.27061","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2026-04-29T18:01:02Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"0da35edb169e33154d02318e4b86b62eabfdc3eb152635afdda9332e40962c04","abstract_canon_sha256":"2479468df79b367a811d1d8d7de32922dddc20d88566f56f58164fcc79034bc7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-06-19T16:10:37.928739Z","signature_b64":"WrRUoiaLqs35d77y6FS5albZClZC8xj2FUQLvVnngB/EKR/DPJQcxGGsbn6xhRwyZPmCfBFDshYupJ6df6seBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"02997d1073020aadff047ebcfda8f7fd2f91b29aa30de02ee735b366e8f26590","last_reissued_at":"2026-06-19T16:10:37.928152Z","signature_status":"signed_v1","first_computed_at":"2026-06-19T16:10:37.928152Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Unveiling the dynamics of the ultra-fast outflow in IRAS 13224-3809 with X-ray spectroscopy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"IRAS 13224-3809 hosts a variable ultra-fast outflow exceeding 0.2c that accelerates rapidly during X-ray flares.","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"Alessia Tortosa, Alfredo Luminari, Enrico Piconcelli, Fabrizio Nicastro, Francesco Tombesi, Giorgio Lanzuisi, Luca Zappacosta, Marco Laurenti, Massimo Gaspari, Pierpaolo Cond\\`o, Riccardo Middei, Roberto Serafinelli","submitted_at":"2026-04-29T18:01:02Z","abstract_excerpt":"IRAS 13224-3809 is one of the most intensively studied narrow-line Seyfert 1 galaxies, with a rich literature reporting diverse and sometimes contrasting interpretations of its complex X-ray spectra and variability. Notably, a fast and variable ultra-fast outflow (UFO) was discovered in this source, sparking debate over its nature and driving mechanisms. Motivated by these open questions, we present a systematic, time- and flux-resolved reanalysis of the full 2016 XMM-Newton (1.5 Ms) and NuSTAR (500 ks) datasets, employing careful background treatment and equal-count spectral selections. We un"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We unambiguously confirm the presence of a strong, variable outflow with velocities exceeding 0.2c, and find that models including absorption consistently reveal robust physical trends: a velocity-luminosity correlation of the UFO, persistently large line widths, and no compelling equivalent-width-flux anti-correlation. We also report clear evidence for rapid acceleration of the wind in response to X-ray flares.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the identified absorption features are correctly attributed to a photo-ionized ultra-fast outflow rather than being mimicked by emission or relativistic reflection components, and that the equal-count spectral selections and background treatment do not introduce systematic biases in the fitted trends.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Reanalysis of 2016 XMM-Newton and NuSTAR data confirms a strong variable ultra-fast outflow in IRAS 13224-3809 with velocities >0.2c, velocity-luminosity correlation, rapid flare response, and evidence favoring magnetic over radiative driving.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"IRAS 13224-3809 hosts a variable ultra-fast outflow exceeding 0.2c that accelerates rapidly during X-ray flares.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"41a688dbbb29af563d03c16e08003ed0c8a11323f1f0c501a8542b918576abda"},"source":{"id":"2604.27061","kind":"arxiv","version":1},"verdict":{"id":"a199d36c-6019-497e-8b68-63cccb40df5d","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-07T10:34:24.598342Z","strongest_claim":"We unambiguously confirm the presence of a strong, variable outflow with velocities exceeding 0.2c, and find that models including absorption consistently reveal robust physical trends: a velocity-luminosity correlation of the UFO, persistently large line widths, and no compelling equivalent-width-flux anti-correlation. We also report clear evidence for rapid acceleration of the wind in response to X-ray flares.","one_line_summary":"Reanalysis of 2016 XMM-Newton and NuSTAR data confirms a strong variable ultra-fast outflow in IRAS 13224-3809 with velocities >0.2c, velocity-luminosity correlation, rapid flare response, and evidence favoring magnetic over radiative driving.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the identified absorption features are correctly attributed to a photo-ionized ultra-fast outflow rather than being mimicked by emission or relativistic reflection components, and that the equal-count spectral selections and background treatment do not introduce systematic biases in the fitted trends.","pith_extraction_headline":"IRAS 13224-3809 hosts a variable ultra-fast outflow exceeding 0.2c that accelerates rapidly during X-ray flares."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.27061/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"ai_meta_artifact","ran_at":"2026-05-20T23:34:49.889358Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T19:36:49.291602Z","status":"completed","version":"1.0.0","findings_count":0}],"snapshot_sha256":"bea2cc2c5b43c634ad159ad56221b5017a06509f2b93a7e0597be7a4c5da0d2f"},"references":{"count":2,"sample":[{"doi":"","year":2014,"title":"An, H., Madsen, K. K., Westergaard, N. J., et al. 2014, in Society of Photo- Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 9144, Space Telescopes and Instrumentation 2014: Ultravio","work_id":"447c3a0d-1227-48d0-a671-8d56944d4155","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2024,"title":"The code requires an ionizing spectral energy distribution (SED) and parameters describing the physical properties of the absorbing gas","work_id":"847e14b8-9ffa-4b25-ac2c-3f572d3a90a7","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":2,"snapshot_sha256":"5b53281870f20ba554dd6d379287f981cafa0b1a757560a3060c6e854940dbde","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"2604.27061","created_at":"2026-06-19T16:10:37.928291+00:00"},{"alias_kind":"arxiv_version","alias_value":"2604.27061v1","created_at":"2026-06-19T16:10:37.928291+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2604.27061","created_at":"2026-06-19T16:10:37.928291+00:00"},{"alias_kind":"pith_short_12","alias_value":"AKMX2EDTAIFK","created_at":"2026-06-19T16:10:37.928291+00:00"},{"alias_kind":"pith_short_16","alias_value":"AKMX2EDTAIFK37YE","created_at":"2026-06-19T16:10:37.928291+00:00"},{"alias_kind":"pith_short_8","alias_value":"AKMX2EDT","created_at":"2026-06-19T16:10:37.928291+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U","json":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U.json","graph_json":"https://pith.science/api/pith-number/AKMX2EDTAIFK37YEP26P3KHX7U/graph.json","events_json":"https://pith.science/api/pith-number/AKMX2EDTAIFK37YEP26P3KHX7U/events.json","paper":"https://pith.science/paper/AKMX2EDT"},"agent_actions":{"view_html":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U","download_json":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U.json","view_paper":"https://pith.science/paper/AKMX2EDT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2604.27061&json=true","fetch_graph":"https://pith.science/api/pith-number/AKMX2EDTAIFK37YEP26P3KHX7U/graph.json","fetch_events":"https://pith.science/api/pith-number/AKMX2EDTAIFK37YEP26P3KHX7U/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U/action/storage_attestation","attest_author":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U/action/author_attestation","sign_citation":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U/action/citation_signature","submit_replication":"https://pith.science/pith/AKMX2EDTAIFK37YEP26P3KHX7U/action/replication_record"}},"created_at":"2026-06-19T16:10:37.928291+00:00","updated_at":"2026-06-19T16:10:37.928291+00:00"}