{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:HN5IIG2RZLJBV7ATLJW7U6YQ6Q","short_pith_number":"pith:HN5IIG2R","schema_version":"1.0","canonical_sha256":"3b7a841b51cad21afc135a6dfa7b10f417470bd8f829ebcd2ef39e1db3c373ae","source":{"kind":"arxiv","id":"1906.11814","version":2},"attestation_state":"computed","paper":{"title":"Local determination of the Hubble constant and the deceleration parameter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Camarena, Valerio Marra","submitted_at":"2019-06-27T17:42:42Z","abstract_excerpt":"The determination of the Hubble constant $H_0$ from the Cosmic Microwave Background by the Planck Collaboration [Aghanim et al. 2018] is in tension at $4.2\\sigma$ with respect to the local determination of $H_0$ by the SH0ES collaboration [Reid et al. 2019]. Here, we improve upon the local determination, which fixes the deceleration parameter to the standard $\\Lambda$CDM model value of $q_0=-0.55$, that is, uses information from observations beyond the local universe. First, we derive the effective calibration prior on the absolute magnitude $M_B$ of Supernovae Ia, which can be used in cosmolo"},"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":"1906.11814","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-06-27T17:42:42Z","cross_cats_sorted":[],"title_canon_sha256":"463157527e210a41a1602ff6eb19ae98a0064355a443d83ea7ab1d3a3a5865b3","abstract_canon_sha256":"7ae4b5c1404557bbdcdd7edd242788fa4c0631a3de4b38ad4f0bf70bde7415f1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:32:30.247183Z","signature_b64":"p8M/MduHzR1LdwPt0kEzYcKAFkX5ygODchLa1p/yMv4OKM5zfTEcgUsYoDeVxlEiFG0jO26J5qt92BaoWGPoAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3b7a841b51cad21afc135a6dfa7b10f417470bd8f829ebcd2ef39e1db3c373ae","last_reissued_at":"2026-07-05T00:32:30.246756Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:32:30.246756Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Local determination of the Hubble constant and the deceleration parameter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Camarena, Valerio Marra","submitted_at":"2019-06-27T17:42:42Z","abstract_excerpt":"The determination of the Hubble constant $H_0$ from the Cosmic Microwave Background by the Planck Collaboration [Aghanim et al. 2018] is in tension at $4.2\\sigma$ with respect to the local determination of $H_0$ by the SH0ES collaboration [Reid et al. 2019]. Here, we improve upon the local determination, which fixes the deceleration parameter to the standard $\\Lambda$CDM model value of $q_0=-0.55$, that is, uses information from observations beyond the local universe. First, we derive the effective calibration prior on the absolute magnitude $M_B$ of Supernovae Ia, which can be used in cosmolo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1906.11814","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1906.11814/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":"1906.11814","created_at":"2026-07-05T00:32:30.246813+00:00"},{"alias_kind":"arxiv_version","alias_value":"1906.11814v2","created_at":"2026-07-05T00:32:30.246813+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1906.11814","created_at":"2026-07-05T00:32:30.246813+00:00"},{"alias_kind":"pith_short_12","alias_value":"HN5IIG2RZLJB","created_at":"2026-07-05T00:32:30.246813+00:00"},{"alias_kind":"pith_short_16","alias_value":"HN5IIG2RZLJBV7AT","created_at":"2026-07-05T00:32:30.246813+00:00"},{"alias_kind":"pith_short_8","alias_value":"HN5IIG2R","created_at":"2026-07-05T00:32:30.246813+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2411.03773","citing_title":"Model-independent calibration of Gamma-Ray Bursts with neural networks","ref_index":79,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11987","citing_title":"Asymptotic Theorems and Averaging in Scalar Field Cosmology","ref_index":67,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q","json":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q.json","graph_json":"https://pith.science/api/pith-number/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/graph.json","events_json":"https://pith.science/api/pith-number/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/events.json","paper":"https://pith.science/paper/HN5IIG2R"},"agent_actions":{"view_html":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q","download_json":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q.json","view_paper":"https://pith.science/paper/HN5IIG2R","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1906.11814&json=true","fetch_graph":"https://pith.science/api/pith-number/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/graph.json","fetch_events":"https://pith.science/api/pith-number/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/action/storage_attestation","attest_author":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/action/author_attestation","sign_citation":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/action/citation_signature","submit_replication":"https://pith.science/pith/HN5IIG2RZLJBV7ATLJW7U6YQ6Q/action/replication_record"}},"created_at":"2026-07-05T00:32:30.246813+00:00","updated_at":"2026-07-05T00:32:30.246813+00:00"}