{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:LLH2GCT46M3YACVDD526CYEEVM","short_pith_number":"pith:LLH2GCT4","schema_version":"1.0","canonical_sha256":"5acfa30a7cf337800aa31f75e16084ab3c883beda34a6d11a797575148604c29","source":{"kind":"arxiv","id":"0804.0909","version":3},"attestation_state":"computed","paper":{"title":"Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) NAOJ, (3) Tokyo), Mamoru Doi (3), Naoki Yasuda (3) ((1) Kyoto, Takeshi Oda (1), Tomoki Morokuma (2), Tomonori Totani (1)","submitted_at":"2008-04-07T11:05:40Z","abstract_excerpt":"The delay time distribution (DTD) of type Ia supernovae (SNe Ia) from star formation is an important clue to reveal the still unknown progenitor system of SNe Ia. Here we report on a measurement of the SN Ia DTD in a delay time range of t_Ia = 0.1-8.0 Gyr by using the faint variable objects detected in the Subaru/XMM-Newton Deep Survey (SXDS) down to i' ~ 25.5. We select 65 SN candidates showing significant spatial offset from nuclei of the host galaxies having old stellar population at z ~ 0.4-1.2, out of more than 1,000 SXDS variable objects. Although spectroscopic type classification is not"},"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":"0804.0909","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-04-07T11:05:40Z","cross_cats_sorted":[],"title_canon_sha256":"c4a12a3ac4bff1e1179e9f41a353b5c5d2db3bc385728c47676ea70d969cac29","abstract_canon_sha256":"4f052bc2d1e3eb1a0b5ac6d832088d983dd295a09628b12a9d3e4884db2905ac"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:15:53.955707Z","signature_b64":"jj/aU7dTcEkrLqVG5qIPj/FHJ2r0QzwzkOU4bJcEwP7yxOtCuCCXBAHGc9PYbK4uawQn3Dyvq69fyxGvBGUSAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5acfa30a7cf337800aa31f75e16084ab3c883beda34a6d11a797575148604c29","last_reissued_at":"2026-05-18T02:15:53.955123Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:15:53.955123Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) NAOJ, (3) Tokyo), Mamoru Doi (3), Naoki Yasuda (3) ((1) Kyoto, Takeshi Oda (1), Tomoki Morokuma (2), Tomonori Totani (1)","submitted_at":"2008-04-07T11:05:40Z","abstract_excerpt":"The delay time distribution (DTD) of type Ia supernovae (SNe Ia) from star formation is an important clue to reveal the still unknown progenitor system of SNe Ia. Here we report on a measurement of the SN Ia DTD in a delay time range of t_Ia = 0.1-8.0 Gyr by using the faint variable objects detected in the Subaru/XMM-Newton Deep Survey (SXDS) down to i' ~ 25.5. We select 65 SN candidates showing significant spatial offset from nuclei of the host galaxies having old stellar population at z ~ 0.4-1.2, out of more than 1,000 SXDS variable objects. Although spectroscopic type classification is not"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0804.0909","kind":"arxiv","version":3},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"0804.0909","created_at":"2026-05-18T02:15:53.955214+00:00"},{"alias_kind":"arxiv_version","alias_value":"0804.0909v3","created_at":"2026-05-18T02:15:53.955214+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0804.0909","created_at":"2026-05-18T02:15:53.955214+00:00"},{"alias_kind":"pith_short_12","alias_value":"LLH2GCT46M3Y","created_at":"2026-05-18T12:25:57.157939+00:00"},{"alias_kind":"pith_short_16","alias_value":"LLH2GCT46M3YACVD","created_at":"2026-05-18T12:25:57.157939+00:00"},{"alias_kind":"pith_short_8","alias_value":"LLH2GCT4","created_at":"2026-05-18T12:25:57.157939+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.12596","citing_title":"Strong Progenitor Age Bias in Supernova Cosmology. III. Progenitor Age as the Physical Origin of the Type Ia Supernova Magnitude Steps with Host Properties","ref_index":98,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM","json":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM.json","graph_json":"https://pith.science/api/pith-number/LLH2GCT46M3YACVDD526CYEEVM/graph.json","events_json":"https://pith.science/api/pith-number/LLH2GCT46M3YACVDD526CYEEVM/events.json","paper":"https://pith.science/paper/LLH2GCT4"},"agent_actions":{"view_html":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM","download_json":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM.json","view_paper":"https://pith.science/paper/LLH2GCT4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0804.0909&json=true","fetch_graph":"https://pith.science/api/pith-number/LLH2GCT46M3YACVDD526CYEEVM/graph.json","fetch_events":"https://pith.science/api/pith-number/LLH2GCT46M3YACVDD526CYEEVM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM/action/storage_attestation","attest_author":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM/action/author_attestation","sign_citation":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM/action/citation_signature","submit_replication":"https://pith.science/pith/LLH2GCT46M3YACVDD526CYEEVM/action/replication_record"}},"created_at":"2026-05-18T02:15:53.955214+00:00","updated_at":"2026-05-18T02:15:53.955214+00:00"}