{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:ZHKTOSBC7PUSEX4U5ZBGAMI76S","short_pith_number":"pith:ZHKTOSBC","schema_version":"1.0","canonical_sha256":"c9d5374822fbe9225f94ee4260311ff4967b0944665a0bc804ffe93da22ddc99","source":{"kind":"arxiv","id":"1901.06269","version":2},"attestation_state":"computed","paper":{"title":"A kilonova associated with GRB 070809","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Da-Ming Wei, Neng-Hui Liao, Paolo D'Avanzo, Stefano Covino, Xiang Li, Yi-Zhong Fan, Zhi-Ping Jin","submitted_at":"2019-01-18T14:36:35Z","abstract_excerpt":"For on-axis typical short gamma-ray bursts (sGRBs), the forward shock emission is usually so bright that renders the identification of kilonovae (also known as macronovae) in the early afterglow ($t<0.5$ d) phase rather challenging. This is why previously no thermal-like kilonova component has been identified at such early time except in the off-axis dim GRB 170817A associated with GW170817. Here we report the identification of an unusual optical radiation component in GRB 070809 at $t\\sim 0.47$ d, thanks plausibly to the very-weak/subdominant forward shock emission. The optical emission with "},"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":"1901.06269","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-01-18T14:36:35Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"8e62ee74a3ca5bee0bf2342e9678c29a3e7a047171916e00a8b050280e908881","abstract_canon_sha256":"a3f133268e88084f9d24b9c36182f2f39e331d445fbc2cdd557b19048320c7fe"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:58:31.778131Z","signature_b64":"x2aIxiGCJiUpG8lpWIB9c40nF81qGdWzAKBpbxwfjwbsFYBWddJGYWHWYJ7FhkQzOdkcDlLxrlv+AA8kvMAYDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c9d5374822fbe9225f94ee4260311ff4967b0944665a0bc804ffe93da22ddc99","last_reissued_at":"2026-07-05T00:58:31.777717Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:58:31.777717Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A kilonova associated with GRB 070809","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Da-Ming Wei, Neng-Hui Liao, Paolo D'Avanzo, Stefano Covino, Xiang Li, Yi-Zhong Fan, Zhi-Ping Jin","submitted_at":"2019-01-18T14:36:35Z","abstract_excerpt":"For on-axis typical short gamma-ray bursts (sGRBs), the forward shock emission is usually so bright that renders the identification of kilonovae (also known as macronovae) in the early afterglow ($t<0.5$ d) phase rather challenging. This is why previously no thermal-like kilonova component has been identified at such early time except in the off-axis dim GRB 170817A associated with GW170817. Here we report the identification of an unusual optical radiation component in GRB 070809 at $t\\sim 0.47$ d, thanks plausibly to the very-weak/subdominant forward shock emission. The optical emission with "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.06269","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1901.06269/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":"1901.06269","created_at":"2026-07-05T00:58:31.777774+00:00"},{"alias_kind":"arxiv_version","alias_value":"1901.06269v2","created_at":"2026-07-05T00:58:31.777774+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1901.06269","created_at":"2026-07-05T00:58:31.777774+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZHKTOSBC7PUS","created_at":"2026-07-05T00:58:31.777774+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZHKTOSBC7PUSEX4U","created_at":"2026-07-05T00:58:31.777774+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZHKTOSBC","created_at":"2026-07-05T00:58:31.777774+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.21392","citing_title":"Kilonova modelling and parameter inference: Understanding uncertainties and evaluating compatibility between observations and models","ref_index":31,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S","json":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S.json","graph_json":"https://pith.science/api/pith-number/ZHKTOSBC7PUSEX4U5ZBGAMI76S/graph.json","events_json":"https://pith.science/api/pith-number/ZHKTOSBC7PUSEX4U5ZBGAMI76S/events.json","paper":"https://pith.science/paper/ZHKTOSBC"},"agent_actions":{"view_html":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S","download_json":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S.json","view_paper":"https://pith.science/paper/ZHKTOSBC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1901.06269&json=true","fetch_graph":"https://pith.science/api/pith-number/ZHKTOSBC7PUSEX4U5ZBGAMI76S/graph.json","fetch_events":"https://pith.science/api/pith-number/ZHKTOSBC7PUSEX4U5ZBGAMI76S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S/action/storage_attestation","attest_author":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S/action/author_attestation","sign_citation":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S/action/citation_signature","submit_replication":"https://pith.science/pith/ZHKTOSBC7PUSEX4U5ZBGAMI76S/action/replication_record"}},"created_at":"2026-07-05T00:58:31.777774+00:00","updated_at":"2026-07-05T00:58:31.777774+00:00"}