{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:4I5SFGUHDEWWKI2GG3VXYP6DIY","short_pith_number":"pith:4I5SFGUH","schema_version":"1.0","canonical_sha256":"e23b229a87192d65234636eb7c3fc34610e8093716b403af5151a6b31c58698d","source":{"kind":"arxiv","id":"1201.6658","version":3},"attestation_state":"computed","paper":{"title":"New constraints on cosmological parameters and neutrino properties using the expansion rate of the Universe to z~1.75","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrea Cimatti, Licia Verde, Lucia Pozzetti, Michele Moresco, Raul Jimenez","submitted_at":"2012-01-31T19:42:22Z","abstract_excerpt":"We have assembled a compilation of observational Hubble parameter measurements estimated with the differential evolution of cosmic chronometers, in the redshift range 0<z<1.75. This sample has been used, in combination with CMB data and with the most recent estimate of the Hubble constant H_0, to derive new constraints on several cosmological parameters. The new Hubble parameter data are very useful to break some of the parameter degeneracies present in CMB-only analysis, and to constrain possible deviations from the standard (minimal) flat \\Lambda CDM model. The H(z) data are especially valua"},"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":"1201.6658","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-01-31T19:42:22Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"ac25940e22db36ea4fe42e1c42c557e363dd1472cf7f20ff5daa00c0cb060523","abstract_canon_sha256":"07b6192bd4366811127463298a9a76fe657f3a6b8d590628025285d1455ff32b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:34:35.713928Z","signature_b64":"UVw7Ra0hCa4jNv8/YE519sVUAQZ7llsvNl4Pe5uKEniOC2bgPBGBhaYE9TQ9wmtrgMeZ1yHkT2F57uOc/PB3DQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e23b229a87192d65234636eb7c3fc34610e8093716b403af5151a6b31c58698d","last_reissued_at":"2026-05-18T03:34:35.713383Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:34:35.713383Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"New constraints on cosmological parameters and neutrino properties using the expansion rate of the Universe to z~1.75","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrea Cimatti, Licia Verde, Lucia Pozzetti, Michele Moresco, Raul Jimenez","submitted_at":"2012-01-31T19:42:22Z","abstract_excerpt":"We have assembled a compilation of observational Hubble parameter measurements estimated with the differential evolution of cosmic chronometers, in the redshift range 0<z<1.75. This sample has been used, in combination with CMB data and with the most recent estimate of the Hubble constant H_0, to derive new constraints on several cosmological parameters. The new Hubble parameter data are very useful to break some of the parameter degeneracies present in CMB-only analysis, and to constrain possible deviations from the standard (minimal) flat \\Lambda CDM model. The H(z) data are especially valua"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1201.6658","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":"1201.6658","created_at":"2026-05-18T03:34:35.713453+00:00"},{"alias_kind":"arxiv_version","alias_value":"1201.6658v3","created_at":"2026-05-18T03:34:35.713453+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1201.6658","created_at":"2026-05-18T03:34:35.713453+00:00"},{"alias_kind":"pith_short_12","alias_value":"4I5SFGUHDEWW","created_at":"2026-05-18T12:26:53.410803+00:00"},{"alias_kind":"pith_short_16","alias_value":"4I5SFGUHDEWWKI2G","created_at":"2026-05-18T12:26:53.410803+00:00"},{"alias_kind":"pith_short_8","alias_value":"4I5SFGUH","created_at":"2026-05-18T12:26:53.410803+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2603.03568","citing_title":"Observational constraints on Luciano-Saridakis entropic cosmology","ref_index":96,"is_internal_anchor":true},{"citing_arxiv_id":"2512.20383","citing_title":"A Spectrum of Cosmological Rips and Their Observational Signatures","ref_index":51,"is_internal_anchor":true},{"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":115,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY","json":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY.json","graph_json":"https://pith.science/api/pith-number/4I5SFGUHDEWWKI2GG3VXYP6DIY/graph.json","events_json":"https://pith.science/api/pith-number/4I5SFGUHDEWWKI2GG3VXYP6DIY/events.json","paper":"https://pith.science/paper/4I5SFGUH"},"agent_actions":{"view_html":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY","download_json":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY.json","view_paper":"https://pith.science/paper/4I5SFGUH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1201.6658&json=true","fetch_graph":"https://pith.science/api/pith-number/4I5SFGUHDEWWKI2GG3VXYP6DIY/graph.json","fetch_events":"https://pith.science/api/pith-number/4I5SFGUHDEWWKI2GG3VXYP6DIY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY/action/storage_attestation","attest_author":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY/action/author_attestation","sign_citation":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY/action/citation_signature","submit_replication":"https://pith.science/pith/4I5SFGUHDEWWKI2GG3VXYP6DIY/action/replication_record"}},"created_at":"2026-05-18T03:34:35.713453+00:00","updated_at":"2026-05-18T03:34:35.713453+00:00"}