{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:HT5BMXGLBU5LFHAQ7BTJEO6TQ7","short_pith_number":"pith:HT5BMXGL","schema_version":"1.0","canonical_sha256":"3cfa165ccb0d3ab29c10f866923bd387e962256976a8d3550b88906481ea47b2","source":{"kind":"arxiv","id":"astro-ph/0703034","version":3},"attestation_state":"computed","paper":{"title":"Model Independent Reconstruction of the Expansion History of the Universe and the Properties of Dark Energy","license":"","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph","authors_text":"Arman Shafieloo","submitted_at":"2007-03-02T19:13:22Z","abstract_excerpt":"We have improved upon the method of smoothing supernovae data to reconstruct the expansion history of the universe, h(z), using two latest datasets, Gold and SNLS. The reconstruction process does not employ any parameterization and is independent of any dark energy model. The reconstructed h(z) is used to derive the distance factor \"A\" up to redshift 0.35 and the results are compared with the given value of \"A\" from detection of baryon acoustic oscillation peak (BAO). We find very good agreement between supernovae observations and the results from BAO for \\Omega_{0m} \\approx 0.276 \\pm 0.023. T"},"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/0703034","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-03-02T19:13:22Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"0e901ab733b4ce163ba0baeb0008227fb13760cc0e6d9c9c1dfd2b5f99ed50a1","abstract_canon_sha256":"39e70beb442775ad3d62ef2bd815a0bc55a97ecdaae0eb47c5380646f7816733"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:39:39.268654Z","signature_b64":"i0cMp5zDW4PYavVvOdeTAS+eilIGlrIpysExoHewBAVLd+kT74st56d7ZWRjn2EzTDimWr7mZsttGHLTtj2tAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3cfa165ccb0d3ab29c10f866923bd387e962256976a8d3550b88906481ea47b2","last_reissued_at":"2026-07-04T15:39:39.268286Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:39:39.268286Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Model Independent Reconstruction of the Expansion History of the Universe and the Properties of Dark Energy","license":"","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph","authors_text":"Arman Shafieloo","submitted_at":"2007-03-02T19:13:22Z","abstract_excerpt":"We have improved upon the method of smoothing supernovae data to reconstruct the expansion history of the universe, h(z), using two latest datasets, Gold and SNLS. The reconstruction process does not employ any parameterization and is independent of any dark energy model. The reconstructed h(z) is used to derive the distance factor \"A\" up to redshift 0.35 and the results are compared with the given value of \"A\" from detection of baryon acoustic oscillation peak (BAO). We find very good agreement between supernovae observations and the results from BAO for \\Omega_{0m} \\approx 0.276 \\pm 0.023. T"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0703034","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0703034/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":"astro-ph/0703034","created_at":"2026-07-04T15:39:39.268360+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0703034v3","created_at":"2026-07-04T15:39:39.268360+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0703034","created_at":"2026-07-04T15:39:39.268360+00:00"},{"alias_kind":"pith_short_12","alias_value":"HT5BMXGLBU5L","created_at":"2026-07-04T15:39:39.268360+00:00"},{"alias_kind":"pith_short_16","alias_value":"HT5BMXGLBU5LFHAQ","created_at":"2026-07-04T15:39:39.268360+00:00"},{"alias_kind":"pith_short_8","alias_value":"HT5BMXGL","created_at":"2026-07-04T15:39:39.268360+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2512.03314","citing_title":"EFT of Dark Energy with Cosmic Chronometers: Reconstructing Background EFT Functions","ref_index":48,"is_internal_anchor":true},{"citing_arxiv_id":"2604.27511","citing_title":"Finding Strongly Lensed Supernovae from Blended Light Curves","ref_index":40,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25813","citing_title":"Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension","ref_index":104,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22372","citing_title":"Testing $\\Lambda$CDM with ANN-Reconstructed Expansion History from Cosmic Chronometers","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2604.12987","citing_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","ref_index":89,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7","json":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7.json","graph_json":"https://pith.science/api/pith-number/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/graph.json","events_json":"https://pith.science/api/pith-number/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/events.json","paper":"https://pith.science/paper/HT5BMXGL"},"agent_actions":{"view_html":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7","download_json":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7.json","view_paper":"https://pith.science/paper/HT5BMXGL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0703034&json=true","fetch_graph":"https://pith.science/api/pith-number/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/graph.json","fetch_events":"https://pith.science/api/pith-number/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/action/storage_attestation","attest_author":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/action/author_attestation","sign_citation":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/action/citation_signature","submit_replication":"https://pith.science/pith/HT5BMXGLBU5LFHAQ7BTJEO6TQ7/action/replication_record"}},"created_at":"2026-07-04T15:39:39.268360+00:00","updated_at":"2026-07-04T15:39:39.268360+00:00"}