{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1996:4NKAO4GWHI5EZLSX6RQI53NQLZ","short_pith_number":"pith:4NKAO4GW","schema_version":"1.0","canonical_sha256":"e3540770d63a3a4cae57f4608eedb05e481e4083a89b2cc6eb75de91ce52b5b3","source":{"kind":"arxiv","id":"astro-ph/9609059","version":1},"attestation_state":"computed","paper":{"title":"The Absolute Luminosities of the Calan/Tololo Type Ia Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Mario Hamuy (CTIO, M.M. Phillips (CTIO), Nicholas B. Suntzeff (CTIO) Jos\\'e Maza (University of Chile), R. Avil\\'es (CTIO), Robert A. Schommer (CTIO), University of Arizona)","submitted_at":"1996-09-07T20:03:04Z","abstract_excerpt":"We examine the absolute luminosities of 29 SNe Ia in the Calan/Tololo survey. We confirm a relation between the peak luminosity of the SNe and the decline rate as measured by the light curve, as suggested by Phillips (1993). We derive linear slopes to this magnitude-decline rate relation in BV(I)kc colors, using a sample with Bmax-Vmax < 0.2 mag. The scatter around this linear relation (and thus the ability to measure SNe Ia distances) ranges from 0.13 mag (in the I band) to 0.17 mag (in the B band). We also find evidence for significant correlations between the absolute magnitudes or the decl"},"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":"astro-ph/9609059","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1996-09-07T20:03:04Z","cross_cats_sorted":[],"title_canon_sha256":"202e3c819d2c0799f785df4a2b7c009e4533053b1c93f8d45bfc8ccdc550ff14","abstract_canon_sha256":"b529020ff1cc518d8905aa774cab527c34711a0c06623b76a8728b0c3c2e8f95"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:09:21.521279Z","signature_b64":"NGosej/IbKrQKQY9x3nw853y/9FaF+3mw9W8QTtrIZWpBandf6dgwuNavSJWV9pnnA4s4jj/XKA0q6sq/rCQBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e3540770d63a3a4cae57f4608eedb05e481e4083a89b2cc6eb75de91ce52b5b3","last_reissued_at":"2026-05-18T01:09:21.520897Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:09:21.520897Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Absolute Luminosities of the Calan/Tololo Type Ia Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Mario Hamuy (CTIO, M.M. Phillips (CTIO), Nicholas B. Suntzeff (CTIO) Jos\\'e Maza (University of Chile), R. Avil\\'es (CTIO), Robert A. Schommer (CTIO), University of Arizona)","submitted_at":"1996-09-07T20:03:04Z","abstract_excerpt":"We examine the absolute luminosities of 29 SNe Ia in the Calan/Tololo survey. We confirm a relation between the peak luminosity of the SNe and the decline rate as measured by the light curve, as suggested by Phillips (1993). We derive linear slopes to this magnitude-decline rate relation in BV(I)kc colors, using a sample with Bmax-Vmax < 0.2 mag. The scatter around this linear relation (and thus the ability to measure SNe Ia distances) ranges from 0.13 mag (in the I band) to 0.17 mag (in the B band). We also find evidence for significant correlations between the absolute magnitudes or the decl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9609059","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":""},"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":"astro-ph/9609059","created_at":"2026-05-18T01:09:21.520958+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9609059v1","created_at":"2026-05-18T01:09:21.520958+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9609059","created_at":"2026-05-18T01:09:21.520958+00:00"},{"alias_kind":"pith_short_12","alias_value":"4NKAO4GWHI5E","created_at":"2026-05-18T12:25:47.700082+00:00"},{"alias_kind":"pith_short_16","alias_value":"4NKAO4GWHI5EZLSX","created_at":"2026-05-18T12:25:47.700082+00:00"},{"alias_kind":"pith_short_8","alias_value":"4NKAO4GW","created_at":"2026-05-18T12:25:47.700082+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":40,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ","json":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ.json","graph_json":"https://pith.science/api/pith-number/4NKAO4GWHI5EZLSX6RQI53NQLZ/graph.json","events_json":"https://pith.science/api/pith-number/4NKAO4GWHI5EZLSX6RQI53NQLZ/events.json","paper":"https://pith.science/paper/4NKAO4GW"},"agent_actions":{"view_html":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ","download_json":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ.json","view_paper":"https://pith.science/paper/4NKAO4GW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9609059&json=true","fetch_graph":"https://pith.science/api/pith-number/4NKAO4GWHI5EZLSX6RQI53NQLZ/graph.json","fetch_events":"https://pith.science/api/pith-number/4NKAO4GWHI5EZLSX6RQI53NQLZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ/action/storage_attestation","attest_author":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ/action/author_attestation","sign_citation":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ/action/citation_signature","submit_replication":"https://pith.science/pith/4NKAO4GWHI5EZLSX6RQI53NQLZ/action/replication_record"}},"created_at":"2026-05-18T01:09:21.520958+00:00","updated_at":"2026-05-18T01:09:21.520958+00:00"}