{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:GWE4MDSXDP6PBD7VWFHGFDHWYZ","short_pith_number":"pith:GWE4MDSX","schema_version":"1.0","canonical_sha256":"3589c60e571bfcf08ff5b14e628cf6c6552c0edf3364a947a6e2640bcd68f96e","source":{"kind":"arxiv","id":"1712.04380","version":1},"attestation_state":"computed","paper":{"title":"Cosmographic analysis with Chebyshev polynomials","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Orlando Luongo, Rocco D'Agostino, Salvatore Capozziello","submitted_at":"2017-12-12T16:36:38Z","abstract_excerpt":"The limits of standard cosmography are here revised addressing the problem of error propagation during statistical analyses. To do so, we propose the use of Chebyshev polynomials to parameterize cosmic distances. In particular, we demonstrate that building up rational Chebyshev polynomials significantly reduces error propagations with respect to standard Taylor series. This technique provides unbiased estimations of the cosmographic parameters and performs significatively better than previous numerical approximations. To figure this out, we compare rational Chebyshev polynomials with Pad\\'e se"},"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":"1712.04380","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-12-12T16:36:38Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"936a3c8514b205ebe9a972d9bef48c08c104991c762e6e66acc227c03c82e4d2","abstract_canon_sha256":"8d564209c467962ce80e2b9c895505b7112b7ebc591323507364a3e8f687d150"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:21:09.071764Z","signature_b64":"oHemMCDkRQzkXzJuF0ir7FH5VpvFXbok9YIdQGFEhMUksZpiaIRQmHhh1qB3uy/I6JS7DSV5ZbRO/JbMEPtjCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3589c60e571bfcf08ff5b14e628cf6c6552c0edf3364a947a6e2640bcd68f96e","last_reissued_at":"2026-05-18T00:21:09.071175Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:21:09.071175Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmographic analysis with Chebyshev polynomials","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Orlando Luongo, Rocco D'Agostino, Salvatore Capozziello","submitted_at":"2017-12-12T16:36:38Z","abstract_excerpt":"The limits of standard cosmography are here revised addressing the problem of error propagation during statistical analyses. To do so, we propose the use of Chebyshev polynomials to parameterize cosmic distances. In particular, we demonstrate that building up rational Chebyshev polynomials significantly reduces error propagations with respect to standard Taylor series. This technique provides unbiased estimations of the cosmographic parameters and performs significatively better than previous numerical approximations. To figure this out, we compare rational Chebyshev polynomials with Pad\\'e se"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1712.04380","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":"1712.04380","created_at":"2026-05-18T00:21:09.071273+00:00"},{"alias_kind":"arxiv_version","alias_value":"1712.04380v1","created_at":"2026-05-18T00:21:09.071273+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1712.04380","created_at":"2026-05-18T00:21:09.071273+00:00"},{"alias_kind":"pith_short_12","alias_value":"GWE4MDSXDP6P","created_at":"2026-05-18T12:31:18.294218+00:00"},{"alias_kind":"pith_short_16","alias_value":"GWE4MDSXDP6PBD7V","created_at":"2026-05-18T12:31:18.294218+00:00"},{"alias_kind":"pith_short_8","alias_value":"GWE4MDSX","created_at":"2026-05-18T12:31:18.294218+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.03167","citing_title":"Mapping the redshift drift at various redshifts through cosmography","ref_index":61,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":88,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ","json":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ.json","graph_json":"https://pith.science/api/pith-number/GWE4MDSXDP6PBD7VWFHGFDHWYZ/graph.json","events_json":"https://pith.science/api/pith-number/GWE4MDSXDP6PBD7VWFHGFDHWYZ/events.json","paper":"https://pith.science/paper/GWE4MDSX"},"agent_actions":{"view_html":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ","download_json":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ.json","view_paper":"https://pith.science/paper/GWE4MDSX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1712.04380&json=true","fetch_graph":"https://pith.science/api/pith-number/GWE4MDSXDP6PBD7VWFHGFDHWYZ/graph.json","fetch_events":"https://pith.science/api/pith-number/GWE4MDSXDP6PBD7VWFHGFDHWYZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ/action/storage_attestation","attest_author":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ/action/author_attestation","sign_citation":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ/action/citation_signature","submit_replication":"https://pith.science/pith/GWE4MDSXDP6PBD7VWFHGFDHWYZ/action/replication_record"}},"created_at":"2026-05-18T00:21:09.071273+00:00","updated_at":"2026-05-18T00:21:09.071273+00:00"}