{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:MQIAZLBGCYAS6VXH5GMSWOYB7Q","short_pith_number":"pith:MQIAZLBG","schema_version":"1.0","canonical_sha256":"64100cac2616012f56e7e9992b3b01fc309c128a5810d59c96444e7e9e629d4e","source":{"kind":"arxiv","id":"1509.07471","version":1},"attestation_state":"computed","paper":{"title":"Towards a cosmological neutrino mass detection","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Erminia Calabrese, Joanna Dunkley, Paul Caucal, Rupert Allison, Thibaut Louis","submitted_at":"2015-09-24T18:46:29Z","abstract_excerpt":"Future cosmological measurements should enable the sum of neutrino masses to be determined indirectly through their effects on the expansion rate of the Universe and the clustering of matter. We consider prospects for the gravitationally lensed Cosmic Microwave Background anisotropies and Baryon Acoustic Oscillations in the galaxy distribution, examining how the projected uncertainty of $\\approx15$ meV on the neutrino mass sum (a 4$\\sigma$ detection of the minimal mass) might be reached over the next decade. The current 1$\\sigma$ uncertainty of $\\approx 103$ meV (Planck-2015+BAO-15) will be im"},"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":"1509.07471","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2015-09-24T18:46:29Z","cross_cats_sorted":[],"title_canon_sha256":"c9869892da3afda596fd7d32959d33ac4d655237429382ca25084b0a3e6b3244","abstract_canon_sha256":"6518736e7b0b8b68cd7a13753637e64eca25c6d78ac97a52e512be262548d0ee"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:23:39.629177Z","signature_b64":"jzZ272hQzcJFt3gWoc5vNanCN6MNgQcp7ItoU9TSL/EFs8c/Yz4WNWteUzJIjgNoJ1chAzOIYRU9huxqTpeMDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"64100cac2616012f56e7e9992b3b01fc309c128a5810d59c96444e7e9e629d4e","last_reissued_at":"2026-05-18T01:23:39.628734Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:23:39.628734Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Towards a cosmological neutrino mass detection","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Erminia Calabrese, Joanna Dunkley, Paul Caucal, Rupert Allison, Thibaut Louis","submitted_at":"2015-09-24T18:46:29Z","abstract_excerpt":"Future cosmological measurements should enable the sum of neutrino masses to be determined indirectly through their effects on the expansion rate of the Universe and the clustering of matter. We consider prospects for the gravitationally lensed Cosmic Microwave Background anisotropies and Baryon Acoustic Oscillations in the galaxy distribution, examining how the projected uncertainty of $\\approx15$ meV on the neutrino mass sum (a 4$\\sigma$ detection of the minimal mass) might be reached over the next decade. The current 1$\\sigma$ uncertainty of $\\approx 103$ meV (Planck-2015+BAO-15) will be im"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1509.07471","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":"1509.07471","created_at":"2026-05-18T01:23:39.628807+00:00"},{"alias_kind":"arxiv_version","alias_value":"1509.07471v1","created_at":"2026-05-18T01:23:39.628807+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1509.07471","created_at":"2026-05-18T01:23:39.628807+00:00"},{"alias_kind":"pith_short_12","alias_value":"MQIAZLBGCYAS","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_16","alias_value":"MQIAZLBGCYAS6VXH","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_8","alias_value":"MQIAZLBG","created_at":"2026-05-18T12:29:32.376354+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"1907.08010","citing_title":"Cosmological searches for the neutrino mass scale and mass ordering","ref_index":12,"is_internal_anchor":true},{"citing_arxiv_id":"2603.10787","citing_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","ref_index":59,"is_internal_anchor":true},{"citing_arxiv_id":"2604.14088","citing_title":"BROOM: a python package for model-independent analysis of microwave astronomical data","ref_index":7,"is_internal_anchor":false},{"citing_arxiv_id":"1807.06209","citing_title":"Planck 2018 results. VI. Cosmological parameters","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2604.15287","citing_title":"Neutrino self-interactions in post-reionization era: Lyman-$\\alpha$, 21-cm and cross-spectra","ref_index":89,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q","json":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q.json","graph_json":"https://pith.science/api/pith-number/MQIAZLBGCYAS6VXH5GMSWOYB7Q/graph.json","events_json":"https://pith.science/api/pith-number/MQIAZLBGCYAS6VXH5GMSWOYB7Q/events.json","paper":"https://pith.science/paper/MQIAZLBG"},"agent_actions":{"view_html":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q","download_json":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q.json","view_paper":"https://pith.science/paper/MQIAZLBG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1509.07471&json=true","fetch_graph":"https://pith.science/api/pith-number/MQIAZLBGCYAS6VXH5GMSWOYB7Q/graph.json","fetch_events":"https://pith.science/api/pith-number/MQIAZLBGCYAS6VXH5GMSWOYB7Q/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q/action/storage_attestation","attest_author":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q/action/author_attestation","sign_citation":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q/action/citation_signature","submit_replication":"https://pith.science/pith/MQIAZLBGCYAS6VXH5GMSWOYB7Q/action/replication_record"}},"created_at":"2026-05-18T01:23:39.628807+00:00","updated_at":"2026-05-18T01:23:39.628807+00:00"}