{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:4A57JMZYKU26SWEZKMZWP2C254","short_pith_number":"pith:4A57JMZY","schema_version":"1.0","canonical_sha256":"e03bf4b3385535e95899533367e85aef36aba96311b380fcdbe6361a83d00e06","source":{"kind":"arxiv","id":"2409.06504","version":1},"attestation_state":"computed","paper":{"title":"Discovery of young, oxygen-rich supernova remnants in PHANGS-MUSE galaxies","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"(2) European Southern Observatory, (3) Kyoto University), Hanindyo Kuncarayakti (1), Joseph P. Anderson (2), Keiichi Maeda (3), Seppo Mattila (1) ((1) University of Turku, Timo Kravtsov (1)","submitted_at":"2024-09-10T13:38:08Z","abstract_excerpt":"Context. Supernova remnants (SNRs) are the late stages of supernovae before their merging into the surrounding medium. Oxygen-rich supernova remnants represent a rare subtype with strong visible light oxygen emission. Aims. We present a new method to detect SNRs exploiting the capabilities of modern visible-light integral-field units based on the shapes of the SNR emission lines. Methods. We search for unresolved shocked regions with broadened emission lines using the medium-resolution integral-field spectrograph MUSE on the Very Large Telescope. The spectral resolving power allows shocked emi"},"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":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2409.06504","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-09-10T13:38:08Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"411845263e3ea4bc4c4d7173396b03fd5b4a7cb8346ded6e6870527cae905699","abstract_canon_sha256":"b0f250d24c9b04985bee82c60f21fa2077760c24c9fe8cb633cc5dcf663da83d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:59:07.174506Z","signature_b64":"tD4eSIO773/WiYyTzH/QAEDrYrfddLA+RJhB8iUiaeUmXUEyycunvUnxicT/axlbtHKQMHkBT5X5MWkopCegBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e03bf4b3385535e95899533367e85aef36aba96311b380fcdbe6361a83d00e06","last_reissued_at":"2026-07-05T11:59:07.174068Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:59:07.174068Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Discovery of young, oxygen-rich supernova remnants in PHANGS-MUSE galaxies","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"(2) European Southern Observatory, (3) Kyoto University), Hanindyo Kuncarayakti (1), Joseph P. Anderson (2), Keiichi Maeda (3), Seppo Mattila (1) ((1) University of Turku, Timo Kravtsov (1)","submitted_at":"2024-09-10T13:38:08Z","abstract_excerpt":"Context. Supernova remnants (SNRs) are the late stages of supernovae before their merging into the surrounding medium. Oxygen-rich supernova remnants represent a rare subtype with strong visible light oxygen emission. Aims. We present a new method to detect SNRs exploiting the capabilities of modern visible-light integral-field units based on the shapes of the SNR emission lines. Methods. We search for unresolved shocked regions with broadened emission lines using the medium-resolution integral-field spectrograph MUSE on the Very Large Telescope. The spectral resolving power allows shocked emi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2409.06504","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2409.06504/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"2409.06504","created_at":"2026-07-05T11:59:07.174120+00:00"},{"alias_kind":"arxiv_version","alias_value":"2409.06504v1","created_at":"2026-07-05T11:59:07.174120+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2409.06504","created_at":"2026-07-05T11:59:07.174120+00:00"},{"alias_kind":"pith_short_12","alias_value":"4A57JMZYKU26","created_at":"2026-07-05T11:59:07.174120+00:00"},{"alias_kind":"pith_short_16","alias_value":"4A57JMZYKU26SWEZ","created_at":"2026-07-05T11:59:07.174120+00:00"},{"alias_kind":"pith_short_8","alias_value":"4A57JMZY","created_at":"2026-07-05T11:59:07.174120+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.00208","citing_title":"JWST Reveals Large Reservoirs of Dust and Ongoing Circumstellar Interaction in SN Ibn/Icn 2023xgo over a Year Post-Explosion","ref_index":92,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254","json":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254.json","graph_json":"https://pith.science/api/pith-number/4A57JMZYKU26SWEZKMZWP2C254/graph.json","events_json":"https://pith.science/api/pith-number/4A57JMZYKU26SWEZKMZWP2C254/events.json","paper":"https://pith.science/paper/4A57JMZY"},"agent_actions":{"view_html":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254","download_json":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254.json","view_paper":"https://pith.science/paper/4A57JMZY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2409.06504&json=true","fetch_graph":"https://pith.science/api/pith-number/4A57JMZYKU26SWEZKMZWP2C254/graph.json","fetch_events":"https://pith.science/api/pith-number/4A57JMZYKU26SWEZKMZWP2C254/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254/action/storage_attestation","attest_author":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254/action/author_attestation","sign_citation":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254/action/citation_signature","submit_replication":"https://pith.science/pith/4A57JMZYKU26SWEZKMZWP2C254/action/replication_record"}},"created_at":"2026-07-05T11:59:07.174120+00:00","updated_at":"2026-07-05T11:59:07.174120+00:00"}