{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:WNE2S2MTFXBDEYQIQY7YVS3UXR","short_pith_number":"pith:WNE2S2MT","schema_version":"1.0","canonical_sha256":"b349a969932dc2326208863f8acb74bc735326487ef14e5120b4652265681930","source":{"kind":"arxiv","id":"2407.15640","version":3},"attestation_state":"computed","paper":{"title":"Impacts of dark energy on weighing neutrinos after DESI BAO","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Guo-Hong Du, Peng-Ju Wu, Tian-Nuo Li, Xin Zhang","submitted_at":"2024-07-22T13:59:21Z","abstract_excerpt":"Recently, DESI has released baryon acoustic oscillation (BAO) data, and DES has also published its five-year supernova (SN) data. These observations, combined with cosmic microwave background (CMB) data, support a dynamically evolving dark energy at a high confidence level. When using cosmological observations to weigh neutrinos, the results of weighing neutrinos will be significantly affected by the measurement of dark energy due to the degeneracy between neutrino mass and the dark-energy equation of state. Therefore, we need to understand how the dynamical evolution of dark energy in the cur"},"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":"2407.15640","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-07-22T13:59:21Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"b16052661b618faf70341d7903832c01b5d7e71ad6af5eda1a91e26437204f29","abstract_canon_sha256":"61b4490e036e138dd6cc3d205985a800bb4481486655b1febfb765fd05146579"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:45:54.041774Z","signature_b64":"qzlsrd7d0IMCYGDyc0MnoA2phU7HZ2ryOjd+VcaH+REPlIEohcRzlF1ugrcwdBX9X/E+C63TqBOKrbo67taTAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b349a969932dc2326208863f8acb74bc735326487ef14e5120b4652265681930","last_reissued_at":"2026-07-05T10:45:54.041257Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:45:54.041257Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impacts of dark energy on weighing neutrinos after DESI BAO","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Guo-Hong Du, Peng-Ju Wu, Tian-Nuo Li, Xin Zhang","submitted_at":"2024-07-22T13:59:21Z","abstract_excerpt":"Recently, DESI has released baryon acoustic oscillation (BAO) data, and DES has also published its five-year supernova (SN) data. These observations, combined with cosmic microwave background (CMB) data, support a dynamically evolving dark energy at a high confidence level. When using cosmological observations to weigh neutrinos, the results of weighing neutrinos will be significantly affected by the measurement of dark energy due to the degeneracy between neutrino mass and the dark-energy equation of state. Therefore, we need to understand how the dynamical evolution of dark energy in the cur"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2407.15640","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/2407.15640/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":"2407.15640","created_at":"2026-07-05T10:45:54.041320+00:00"},{"alias_kind":"arxiv_version","alias_value":"2407.15640v3","created_at":"2026-07-05T10:45:54.041320+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2407.15640","created_at":"2026-07-05T10:45:54.041320+00:00"},{"alias_kind":"pith_short_12","alias_value":"WNE2S2MTFXBD","created_at":"2026-07-05T10:45:54.041320+00:00"},{"alias_kind":"pith_short_16","alias_value":"WNE2S2MTFXBDEYQI","created_at":"2026-07-05T10:45:54.041320+00:00"},{"alias_kind":"pith_short_8","alias_value":"WNE2S2MT","created_at":"2026-07-05T10:45:54.041320+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":10,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.21518","citing_title":"Are Cosmological Data Excluding Sterile Neutrinos or Only the Fully Thermalized Limit?","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2606.19090","citing_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","ref_index":91,"is_internal_anchor":false},{"citing_arxiv_id":"2606.17994","citing_title":"Constraints on the Sum of Neutrino Masses from ACT DR6 and DESI DR2 Considering Isocurvature Initial Conditions","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05005","citing_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","ref_index":120,"is_internal_anchor":false},{"citing_arxiv_id":"2510.21521","citing_title":"Synergy between CSST and third-generation gravitational-wave detectors: Inferring cosmological parameters using cross-correlation of dark sirens and galaxies","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2601.02077","citing_title":"Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity","ref_index":64,"is_internal_anchor":false},{"citing_arxiv_id":"2602.03110","citing_title":"Evidence for deviation in gravitational light deflection from general relativity at cosmological scales with KiDS-Legacy and CMB lensing","ref_index":45,"is_internal_anchor":false},{"citing_arxiv_id":"2603.10787","citing_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","ref_index":98,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11956","citing_title":"Probing the small-scale primordial power spectrum via relic neutrinos and acoustic reheating","ref_index":71,"is_internal_anchor":false},{"citing_arxiv_id":"2604.23492","citing_title":"The open-Universe signal: A model artifact rather than genuine curvature","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR","json":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR.json","graph_json":"https://pith.science/api/pith-number/WNE2S2MTFXBDEYQIQY7YVS3UXR/graph.json","events_json":"https://pith.science/api/pith-number/WNE2S2MTFXBDEYQIQY7YVS3UXR/events.json","paper":"https://pith.science/paper/WNE2S2MT"},"agent_actions":{"view_html":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR","download_json":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR.json","view_paper":"https://pith.science/paper/WNE2S2MT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2407.15640&json=true","fetch_graph":"https://pith.science/api/pith-number/WNE2S2MTFXBDEYQIQY7YVS3UXR/graph.json","fetch_events":"https://pith.science/api/pith-number/WNE2S2MTFXBDEYQIQY7YVS3UXR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR/action/storage_attestation","attest_author":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR/action/author_attestation","sign_citation":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR/action/citation_signature","submit_replication":"https://pith.science/pith/WNE2S2MTFXBDEYQIQY7YVS3UXR/action/replication_record"}},"created_at":"2026-07-05T10:45:54.041320+00:00","updated_at":"2026-07-05T10:45:54.041320+00:00"}