{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:SJHTH6X3IDLMU4XM62V42Q6DW6","short_pith_number":"pith:SJHTH6X3","schema_version":"1.0","canonical_sha256":"924f33fafb40d6ca72ecf6abcd43c3b79fd6ed3c750f8317d94ea12d3c53acb3","source":{"kind":"arxiv","id":"1709.02356","version":2},"attestation_state":"computed","paper":{"title":"Constraining the dark energy models with H(z) data: an approach independent of $H_{0}$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Fotios Anagnostopoulos, Spyros Basilakos","submitted_at":"2017-09-07T17:03:18Z","abstract_excerpt":"We study the performance of the latest $H(z)$ data in constraining the cosmological parameters of different cosmological models, including that of Chevalier-Polarski-Linder $w_{0}w_{1}$ parametrization. First, we introduce a statistical procedure in which the chi-square estimator is not affected by the value of the Hubble constant. As a result, we find that the $H(z)$ data do not rule out the possibility of either non-flat models or dynamical dark energy cosmological models. However, we verify that the time varying equation of state parameter $w(z)$ is not constrained by the current expansion "},"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":"1709.02356","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-09-07T17:03:18Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"93a88d0ca1541791c4789d9b72705c5823910990419f3334e3c0868a81f32630","abstract_canon_sha256":"584b0ec2ff1d036f68e20ccdf790f577070ecbf9757810d7db1fecafe59cfb39"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:21:54.686281Z","signature_b64":"uO8x+TkfZ986nnWILTvibv5vPBGqgv5xnczhS6xHCm+yqv9xjtA7bLDstzBvsJmFG6FW2FptwNAtj2tpYNrGCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"924f33fafb40d6ca72ecf6abcd43c3b79fd6ed3c750f8317d94ea12d3c53acb3","last_reissued_at":"2026-05-18T00:21:54.685746Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:21:54.685746Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining the dark energy models with H(z) data: an approach independent of $H_{0}$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Fotios Anagnostopoulos, Spyros Basilakos","submitted_at":"2017-09-07T17:03:18Z","abstract_excerpt":"We study the performance of the latest $H(z)$ data in constraining the cosmological parameters of different cosmological models, including that of Chevalier-Polarski-Linder $w_{0}w_{1}$ parametrization. First, we introduce a statistical procedure in which the chi-square estimator is not affected by the value of the Hubble constant. As a result, we find that the $H(z)$ data do not rule out the possibility of either non-flat models or dynamical dark energy cosmological models. However, we verify that the time varying equation of state parameter $w(z)$ is not constrained by the current expansion "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1709.02356","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":"1709.02356","created_at":"2026-05-18T00:21:54.685820+00:00"},{"alias_kind":"arxiv_version","alias_value":"1709.02356v2","created_at":"2026-05-18T00:21:54.685820+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1709.02356","created_at":"2026-05-18T00:21:54.685820+00:00"},{"alias_kind":"pith_short_12","alias_value":"SJHTH6X3IDLM","created_at":"2026-05-18T12:31:43.269735+00:00"},{"alias_kind":"pith_short_16","alias_value":"SJHTH6X3IDLMU4XM","created_at":"2026-05-18T12:31:43.269735+00:00"},{"alias_kind":"pith_short_8","alias_value":"SJHTH6X3","created_at":"2026-05-18T12:31:43.269735+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.22006","citing_title":"Updated constraints on Regge-Teitelboim gravity","ref_index":12,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6","json":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6.json","graph_json":"https://pith.science/api/pith-number/SJHTH6X3IDLMU4XM62V42Q6DW6/graph.json","events_json":"https://pith.science/api/pith-number/SJHTH6X3IDLMU4XM62V42Q6DW6/events.json","paper":"https://pith.science/paper/SJHTH6X3"},"agent_actions":{"view_html":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6","download_json":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6.json","view_paper":"https://pith.science/paper/SJHTH6X3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1709.02356&json=true","fetch_graph":"https://pith.science/api/pith-number/SJHTH6X3IDLMU4XM62V42Q6DW6/graph.json","fetch_events":"https://pith.science/api/pith-number/SJHTH6X3IDLMU4XM62V42Q6DW6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6/action/storage_attestation","attest_author":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6/action/author_attestation","sign_citation":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6/action/citation_signature","submit_replication":"https://pith.science/pith/SJHTH6X3IDLMU4XM62V42Q6DW6/action/replication_record"}},"created_at":"2026-05-18T00:21:54.685820+00:00","updated_at":"2026-05-18T00:21:54.685820+00:00"}