{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:PCTAET4KIOODBHZXUWAZXCOUCG","short_pith_number":"pith:PCTAET4K","schema_version":"1.0","canonical_sha256":"78a6024f8a439c309f37a5819b89d4119506395028d806f0c573ef89b6bfbee5","source":{"kind":"arxiv","id":"1907.00179","version":3},"attestation_state":"computed","paper":{"title":"Forecast for weighing neutrinos in cosmology with SKA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Bo Wang, Jing-Fei Zhang, Xin Zhang","submitted_at":"2019-06-29T10:47:01Z","abstract_excerpt":"We investigate what role the SKA neutral hydrogen (HI) intensity mapping (IM) sky survey observation will play in weighing neutrinos in cosmology. We use the simulated data of the baryon acoustic oscillation (BAO) measurements from the HI IM survey based on SKA1 and SKA2 to do the analysis. For the current observations, we use the Planck 2015 cosmic microwave background (CMB) anisotropies observation, the optical BAO measurements, the type Ia supernovae (SN) observation (Pantheon compilation), and the latest $H_0$ measurement. We consider three mass ordering cases for massive neutrinos, i.e., "},"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":"1907.00179","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-06-29T10:47:01Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"fbe33164d60bb5e7f333afecc3ebbdf9b3946e6982a53164f95a53b325d8396c","abstract_canon_sha256":"7f051448c4347327f4c4f3fe85c8af09ec6ab21efb648404dd7e103fc93116db"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:55:27.930923Z","signature_b64":"EUkTV+Gx5bDSO5UjsT1XfOROhXCXtie2rHECA55/g2oDDB0+Jh/jWOwm7yNJIIjUwDzfHIVV3s/gr+zucO2CAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"78a6024f8a439c309f37a5819b89d4119506395028d806f0c573ef89b6bfbee5","last_reissued_at":"2026-07-05T00:55:27.930443Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:55:27.930443Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Forecast for weighing neutrinos in cosmology with SKA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Bo Wang, Jing-Fei Zhang, Xin Zhang","submitted_at":"2019-06-29T10:47:01Z","abstract_excerpt":"We investigate what role the SKA neutral hydrogen (HI) intensity mapping (IM) sky survey observation will play in weighing neutrinos in cosmology. We use the simulated data of the baryon acoustic oscillation (BAO) measurements from the HI IM survey based on SKA1 and SKA2 to do the analysis. For the current observations, we use the Planck 2015 cosmic microwave background (CMB) anisotropies observation, the optical BAO measurements, the type Ia supernovae (SN) observation (Pantheon compilation), and the latest $H_0$ measurement. We consider three mass ordering cases for massive neutrinos, i.e., "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.00179","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1907.00179/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":"1907.00179","created_at":"2026-07-05T00:55:27.930501+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.00179v3","created_at":"2026-07-05T00:55:27.930501+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.00179","created_at":"2026-07-05T00:55:27.930501+00:00"},{"alias_kind":"pith_short_12","alias_value":"PCTAET4KIOOD","created_at":"2026-07-05T00:55:27.930501+00:00"},{"alias_kind":"pith_short_16","alias_value":"PCTAET4KIOODBHZX","created_at":"2026-07-05T00:55:27.930501+00:00"},{"alias_kind":"pith_short_8","alias_value":"PCTAET4K","created_at":"2026-07-05T00:55:27.930501+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.05005","citing_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","ref_index":107,"is_internal_anchor":false},{"citing_arxiv_id":"2606.28175","citing_title":"HIcosmo: a differentiable JAX-based framework for cosmology inference","ref_index":70,"is_internal_anchor":false},{"citing_arxiv_id":"2603.10787","citing_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","ref_index":86,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG","json":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG.json","graph_json":"https://pith.science/api/pith-number/PCTAET4KIOODBHZXUWAZXCOUCG/graph.json","events_json":"https://pith.science/api/pith-number/PCTAET4KIOODBHZXUWAZXCOUCG/events.json","paper":"https://pith.science/paper/PCTAET4K"},"agent_actions":{"view_html":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG","download_json":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG.json","view_paper":"https://pith.science/paper/PCTAET4K","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.00179&json=true","fetch_graph":"https://pith.science/api/pith-number/PCTAET4KIOODBHZXUWAZXCOUCG/graph.json","fetch_events":"https://pith.science/api/pith-number/PCTAET4KIOODBHZXUWAZXCOUCG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG/action/storage_attestation","attest_author":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG/action/author_attestation","sign_citation":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG/action/citation_signature","submit_replication":"https://pith.science/pith/PCTAET4KIOODBHZXUWAZXCOUCG/action/replication_record"}},"created_at":"2026-07-05T00:55:27.930501+00:00","updated_at":"2026-07-05T00:55:27.930501+00:00"}