{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:N7FYCKHKYPSZTWZKAEF6ASV3NQ","short_pith_number":"pith:N7FYCKHK","schema_version":"1.0","canonical_sha256":"6fcb8128eac3e599db2a010be04abb6c3dbfa9a73fe53822a0c808c9799144f6","source":{"kind":"arxiv","id":"0912.0929","version":3},"attestation_state":"computed","paper":{"title":"Hubble Residuals of Nearby Type Ia Supernovae Are Correlated with Host Galaxy Masses","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"2), (2) KIPAC, (3) CfA), David L. Burke (1, Kaisey S. Mandel (3), Malcolm Hicken (3), Patrick L. Kelly (1, Robert P. Kirshner (3) ((1) Stanford","submitted_at":"2009-12-04T20:58:27Z","abstract_excerpt":"From Sloan Digital Sky Survey u'g'r'i'z' imaging, we estimate the stellar masses of the host galaxies of 70 low redshift SN Ia (0.015 < z < 0.08) from the hosts' absolute luminosities and mass-to-light ratios. These nearby SN were discovered largely by searches targeting luminous galaxies, and we find that their host galaxies are substantially more massive than the hosts of SN discovered by the flux-limited Supernova Legacy Survey. Testing four separate light curve fitters, we detect ~2.5{\\sigma} correlations of Hubble residuals with both host galaxy size and stellar mass, such that SN Ia occu"},"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":"0912.0929","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-12-04T20:58:27Z","cross_cats_sorted":[],"title_canon_sha256":"eee27a970e11e360310de3a8641569137acafcf6fd1abed0d56abbd4777a802d","abstract_canon_sha256":"d020df55ac9d1b7420687a4bbb91a16b14d794c309b9f83b1be4abe4f2f926b8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:34:02.261793Z","signature_b64":"HOjvrmL+uHbiVX7Gg9XOvK1Zlj7bgnejwX0wyBzqIni19rUZvrXezdrY79VU99sA+M1dNrtxwiMINT8ykK8eAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6fcb8128eac3e599db2a010be04abb6c3dbfa9a73fe53822a0c808c9799144f6","last_reissued_at":"2026-05-18T02:34:02.261331Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:34:02.261331Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Hubble Residuals of Nearby Type Ia Supernovae Are Correlated with Host Galaxy Masses","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"2), (2) KIPAC, (3) CfA), David L. Burke (1, Kaisey S. Mandel (3), Malcolm Hicken (3), Patrick L. Kelly (1, Robert P. Kirshner (3) ((1) Stanford","submitted_at":"2009-12-04T20:58:27Z","abstract_excerpt":"From Sloan Digital Sky Survey u'g'r'i'z' imaging, we estimate the stellar masses of the host galaxies of 70 low redshift SN Ia (0.015 < z < 0.08) from the hosts' absolute luminosities and mass-to-light ratios. These nearby SN were discovered largely by searches targeting luminous galaxies, and we find that their host galaxies are substantially more massive than the hosts of SN discovered by the flux-limited Supernova Legacy Survey. Testing four separate light curve fitters, we detect ~2.5{\\sigma} correlations of Hubble residuals with both host galaxy size and stellar mass, such that SN Ia occu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0912.0929","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":"0912.0929","created_at":"2026-05-18T02:34:02.261406+00:00"},{"alias_kind":"arxiv_version","alias_value":"0912.0929v3","created_at":"2026-05-18T02:34:02.261406+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0912.0929","created_at":"2026-05-18T02:34:02.261406+00:00"},{"alias_kind":"pith_short_12","alias_value":"N7FYCKHKYPSZ","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"N7FYCKHKYPSZTWZK","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"N7FYCKHK","created_at":"2026-05-18T12:26:00.592388+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":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ","json":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ.json","graph_json":"https://pith.science/api/pith-number/N7FYCKHKYPSZTWZKAEF6ASV3NQ/graph.json","events_json":"https://pith.science/api/pith-number/N7FYCKHKYPSZTWZKAEF6ASV3NQ/events.json","paper":"https://pith.science/paper/N7FYCKHK"},"agent_actions":{"view_html":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ","download_json":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ.json","view_paper":"https://pith.science/paper/N7FYCKHK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0912.0929&json=true","fetch_graph":"https://pith.science/api/pith-number/N7FYCKHKYPSZTWZKAEF6ASV3NQ/graph.json","fetch_events":"https://pith.science/api/pith-number/N7FYCKHKYPSZTWZKAEF6ASV3NQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ/action/storage_attestation","attest_author":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ/action/author_attestation","sign_citation":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ/action/citation_signature","submit_replication":"https://pith.science/pith/N7FYCKHKYPSZTWZKAEF6ASV3NQ/action/replication_record"}},"created_at":"2026-05-18T02:34:02.261406+00:00","updated_at":"2026-05-18T02:34:02.261406+00:00"}