{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:2PVB7RZPWMJLGQP5LO4PFKXNCT","short_pith_number":"pith:2PVB7RZP","schema_version":"1.0","canonical_sha256":"d3ea1fc72fb312b341fd5bb8f2aaed14c98034f3390585901e84cde05beb02fe","source":{"kind":"arxiv","id":"1810.06561","version":1},"attestation_state":"computed","paper":{"title":"Measurement of the primordial helium abundance from the intergalactic medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"2) ((1) Centre for Extragalactic Astronomy, (2) Institute for Computational Cosmology, Durham University, Durham University), Michele Fumagalli (1, Ryan Cooke (1)","submitted_at":"2018-10-15T18:00:00Z","abstract_excerpt":"Almost every helium atom in the Universe was created just a few minutes after the Big Bang through a process commonly referred to as Big Bang Nucleosynthesis. The amount of helium that was made during Big Bang Nucleosynthesis is determined by the combination of particle physics and cosmology. The current leading measures of the primordial helium abundance (Y_P) are based on the relative strengths of H I and He I emission lines emanating from star-forming regions in local metal-poor galaxies. As the statistical errors on these measurements improve, it is essential to test for systematics by dev"},"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":"1810.06561","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-10-15T18:00:00Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"139e0d242a7993a53d35a529ba26865bbb436820d37f9417040e182f2f68070f","abstract_canon_sha256":"4a0ad65771c4ba8052de9b274cb3aa232d83dd693689ade2ca6f00a67b445cd6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:03:14.201154Z","signature_b64":"cs6kbv3Z8rDT/UY8tvhTXl+c0dMbEy0WfFyAH4Q59vB49PFfOwU4IzsgoUCuVO2PFi0U9kfuCnfncmUYWBMRBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d3ea1fc72fb312b341fd5bb8f2aaed14c98034f3390585901e84cde05beb02fe","last_reissued_at":"2026-05-18T00:03:14.200547Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:03:14.200547Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measurement of the primordial helium abundance from the intergalactic medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"2) ((1) Centre for Extragalactic Astronomy, (2) Institute for Computational Cosmology, Durham University, Durham University), Michele Fumagalli (1, Ryan Cooke (1)","submitted_at":"2018-10-15T18:00:00Z","abstract_excerpt":"Almost every helium atom in the Universe was created just a few minutes after the Big Bang through a process commonly referred to as Big Bang Nucleosynthesis. The amount of helium that was made during Big Bang Nucleosynthesis is determined by the combination of particle physics and cosmology. The current leading measures of the primordial helium abundance (Y_P) are based on the relative strengths of H I and He I emission lines emanating from star-forming regions in local metal-poor galaxies. As the statistical errors on these measurements improve, it is essential to test for systematics by dev"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.06561","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":"1810.06561","created_at":"2026-05-18T00:03:14.200664+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.06561v1","created_at":"2026-05-18T00:03:14.200664+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.06561","created_at":"2026-05-18T00:03:14.200664+00:00"},{"alias_kind":"pith_short_12","alias_value":"2PVB7RZPWMJL","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_16","alias_value":"2PVB7RZPWMJLGQP5","created_at":"2026-05-18T12:32:02.567920+00:00"},{"alias_kind":"pith_short_8","alias_value":"2PVB7RZP","created_at":"2026-05-18T12:32:02.567920+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.24089","citing_title":"Exploring the Dark Sector: Interacting Radiation in Light of Modern Cosmological Probes","ref_index":72,"is_internal_anchor":true},{"citing_arxiv_id":"2606.03192","citing_title":"Fifty years of primordial helium abundances: A statistical reanalysis","ref_index":134,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25890","citing_title":"Cosmic evolution of the helium and oxygen abundances in type 2 Active Galactic Nuclei: Helium-loud AGNs","ref_index":233,"is_internal_anchor":true},{"citing_arxiv_id":"2509.09202","citing_title":"Interacting $k$-essence field with non-pressureless Dark Matter: Cosmological Dynamics and Observational Constraints","ref_index":98,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT","json":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT.json","graph_json":"https://pith.science/api/pith-number/2PVB7RZPWMJLGQP5LO4PFKXNCT/graph.json","events_json":"https://pith.science/api/pith-number/2PVB7RZPWMJLGQP5LO4PFKXNCT/events.json","paper":"https://pith.science/paper/2PVB7RZP"},"agent_actions":{"view_html":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT","download_json":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT.json","view_paper":"https://pith.science/paper/2PVB7RZP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.06561&json=true","fetch_graph":"https://pith.science/api/pith-number/2PVB7RZPWMJLGQP5LO4PFKXNCT/graph.json","fetch_events":"https://pith.science/api/pith-number/2PVB7RZPWMJLGQP5LO4PFKXNCT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT/action/storage_attestation","attest_author":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT/action/author_attestation","sign_citation":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT/action/citation_signature","submit_replication":"https://pith.science/pith/2PVB7RZPWMJLGQP5LO4PFKXNCT/action/replication_record"}},"created_at":"2026-05-18T00:03:14.200664+00:00","updated_at":"2026-05-18T00:03:14.200664+00:00"}