{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:NDLKPQ7DBF3HGAMASRUE7FDYAR","short_pith_number":"pith:NDLKPQ7D","schema_version":"1.0","canonical_sha256":"68d6a7c3e3097673018094684f9478044ec45de74222dc178565d1fa37d1f1a5","source":{"kind":"arxiv","id":"0707.0690","version":2},"attestation_state":"computed","paper":{"title":"Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"John F. Beacom (Ohio State), Jose L. Prieto, Krzysztof Z. Stanek","submitted_at":"2007-07-05T16:22:48Z","abstract_excerpt":"We investigate how the different types of supernovae are relatively affected by the metallicity of their host galaxy. We match the SAI Supernova Catalog to the SDSS-DR4 catalog of star-forming galaxies with measured metallicities. These supernova host galaxies span a range of oxygen abundance from 12 + log(O/H) = 7.9 to 9.3 (~ 0.1 to 2.7 solar) and a range in absolute magnitude from MB = -15.2 to -22.2. To reduce the various observational biases, we select a subsample of well-characterized supernovae in the redshift range from 0.01 to 0.04, which leaves us with 58 SN II, 19 Ib/c, and 38 Ia. We"},"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":"0707.0690","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-07-05T16:22:48Z","cross_cats_sorted":[],"title_canon_sha256":"f9128b3d022b26f290ca528294c89ba7d42cc466874e0964748ff4a8459e2caa","abstract_canon_sha256":"c7635411b02b1c61182dcf0d1cb74e65a1b4892cc773e6b630efcd418fcc57f2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:36:42.110330Z","signature_b64":"ZeFxux3/aMKMiv8EQNBCwCDMmMRLqB4jr4NQ6Mpci0axXEx/th3nxyBvtNPhuuc9RG/yAwWrk96BfocY0tnjAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"68d6a7c3e3097673018094684f9478044ec45de74222dc178565d1fa37d1f1a5","last_reissued_at":"2026-05-18T04:36:42.109615Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:36:42.109615Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"John F. Beacom (Ohio State), Jose L. Prieto, Krzysztof Z. Stanek","submitted_at":"2007-07-05T16:22:48Z","abstract_excerpt":"We investigate how the different types of supernovae are relatively affected by the metallicity of their host galaxy. We match the SAI Supernova Catalog to the SDSS-DR4 catalog of star-forming galaxies with measured metallicities. These supernova host galaxies span a range of oxygen abundance from 12 + log(O/H) = 7.9 to 9.3 (~ 0.1 to 2.7 solar) and a range in absolute magnitude from MB = -15.2 to -22.2. To reduce the various observational biases, we select a subsample of well-characterized supernovae in the redshift range from 0.01 to 0.04, which leaves us with 58 SN II, 19 Ib/c, and 38 Ia. We"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0707.0690","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":""},"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":"0707.0690","created_at":"2026-05-18T04:36:42.109737+00:00"},{"alias_kind":"arxiv_version","alias_value":"0707.0690v2","created_at":"2026-05-18T04:36:42.109737+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0707.0690","created_at":"2026-05-18T04:36:42.109737+00:00"},{"alias_kind":"pith_short_12","alias_value":"NDLKPQ7DBF3H","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_16","alias_value":"NDLKPQ7DBF3HGAMA","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_8","alias_value":"NDLKPQ7D","created_at":"2026-05-18T12:25:55.427421+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21062","citing_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","ref_index":296,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR","json":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR.json","graph_json":"https://pith.science/api/pith-number/NDLKPQ7DBF3HGAMASRUE7FDYAR/graph.json","events_json":"https://pith.science/api/pith-number/NDLKPQ7DBF3HGAMASRUE7FDYAR/events.json","paper":"https://pith.science/paper/NDLKPQ7D"},"agent_actions":{"view_html":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR","download_json":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR.json","view_paper":"https://pith.science/paper/NDLKPQ7D","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0707.0690&json=true","fetch_graph":"https://pith.science/api/pith-number/NDLKPQ7DBF3HGAMASRUE7FDYAR/graph.json","fetch_events":"https://pith.science/api/pith-number/NDLKPQ7DBF3HGAMASRUE7FDYAR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR/action/storage_attestation","attest_author":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR/action/author_attestation","sign_citation":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR/action/citation_signature","submit_replication":"https://pith.science/pith/NDLKPQ7DBF3HGAMASRUE7FDYAR/action/replication_record"}},"created_at":"2026-05-18T04:36:42.109737+00:00","updated_at":"2026-05-18T04:36:42.109737+00:00"}