{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:QNWSP4LSN5GESJA3VZ4B727DBA","short_pith_number":"pith:QNWSP4LS","schema_version":"1.0","canonical_sha256":"836d27f1726f4c49241bae781febe3082dfecb018202c666cb2da0bfb2042baa","source":{"kind":"arxiv","id":"2504.21813","version":1},"attestation_state":"computed","paper":{"title":"Turning a negative neutrino mass into a positive optical depth","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Tanisha Jhaveri, Tanvi Karwal, Wayne Hu","submitted_at":"2025-04-30T17:16:54Z","abstract_excerpt":"Under $\\Lambda$CDM, recent baryon acoustic oscillation (BAO) distance measures from DESI, which favor a low matter density $\\Omega_m$, are in moderate $2-3\\sigma$ tension with cosmic microwave background (CMB) observations. This tension appears alternately as a preference for the sum of neutrino masses dropping below the $\\sum m_\\nu = 0.06$eV value required by neutrino oscillation measurements to formally negative values; a discrepant value of $\\Omega_m$ at 0.06eV; or preference for dynamical dark energy beyond $\\Lambda$CDM. We show that this tension largely arises from the CMB lensing constra"},"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":"2504.21813","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-04-30T17:16:54Z","cross_cats_sorted":[],"title_canon_sha256":"c73106d163e27f589e041826a8c5a950ce87da15e942de8cbbd1c1de928a704e","abstract_canon_sha256":"26db8e112b3e30c315192f28aa1f4c776c5c759e38e8769aa01798d2d0adfc4c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:56:29.777961Z","signature_b64":"w/s+XAgqT8026yp2GGl0NgEVMqMfhW4u/gW5xQrFQmjVpbUuGafdj1tWWvTmSN2csWTlYvIM5WAaAgZYe+4QCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"836d27f1726f4c49241bae781febe3082dfecb018202c666cb2da0bfb2042baa","last_reissued_at":"2026-07-05T10:56:29.777493Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:56:29.777493Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Turning a negative neutrino mass into a positive optical depth","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Tanisha Jhaveri, Tanvi Karwal, Wayne Hu","submitted_at":"2025-04-30T17:16:54Z","abstract_excerpt":"Under $\\Lambda$CDM, recent baryon acoustic oscillation (BAO) distance measures from DESI, which favor a low matter density $\\Omega_m$, are in moderate $2-3\\sigma$ tension with cosmic microwave background (CMB) observations. This tension appears alternately as a preference for the sum of neutrino masses dropping below the $\\sum m_\\nu = 0.06$eV value required by neutrino oscillation measurements to formally negative values; a discrepant value of $\\Omega_m$ at 0.06eV; or preference for dynamical dark energy beyond $\\Lambda$CDM. We show that this tension largely arises from the CMB lensing constra"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2504.21813","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2504.21813/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":"2504.21813","created_at":"2026-07-05T10:56:29.777551+00:00"},{"alias_kind":"arxiv_version","alias_value":"2504.21813v1","created_at":"2026-07-05T10:56:29.777551+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2504.21813","created_at":"2026-07-05T10:56:29.777551+00:00"},{"alias_kind":"pith_short_12","alias_value":"QNWSP4LSN5GE","created_at":"2026-07-05T10:56:29.777551+00:00"},{"alias_kind":"pith_short_16","alias_value":"QNWSP4LSN5GESJA3","created_at":"2026-07-05T10:56:29.777551+00:00"},{"alias_kind":"pith_short_8","alias_value":"QNWSP4LS","created_at":"2026-07-05T10:56:29.777551+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":14,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07777","citing_title":"The Status of Single Scalar Field Dark Energy","ref_index":80,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20795","citing_title":"Raising the reionization optical depth with inflationary CMB features","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2606.19449","citing_title":"A self-consistent analytical model for both the photoionization rate and reionization history","ref_index":109,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05853","citing_title":"Reconstructing dark energy with fewer assumptions","ref_index":86,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05166","citing_title":"Compressed Gaussian likelihood for the Planck low-$\\ell$ data","ref_index":15,"is_internal_anchor":false},{"citing_arxiv_id":"2607.01226","citing_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","ref_index":185,"is_internal_anchor":false},{"citing_arxiv_id":"2606.27903","citing_title":"A hidden reionization prior biases cosmological inference","ref_index":30,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31324","citing_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","ref_index":225,"is_internal_anchor":false},{"citing_arxiv_id":"2606.30903","citing_title":"Cosmological Concordance in an Especially Opaque Universe: A Tentative Cosmological Detection of Physical Neutrino Mass in $\\Lambda$CDM","ref_index":53,"is_internal_anchor":false},{"citing_arxiv_id":"2605.18659","citing_title":"Faster CMB lensing with control variates","ref_index":31,"is_internal_anchor":false},{"citing_arxiv_id":"2506.23290","citing_title":"Type II Seesaw Leptogenesis in a Majoron background","ref_index":105,"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":111,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13423","citing_title":"Into the Gompverse: A robust Gompertzian reionization model for CMB analyses","ref_index":9,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08530","citing_title":"Disentangling cosmic distance tensions with early and late dark energy","ref_index":52,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA","json":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA.json","graph_json":"https://pith.science/api/pith-number/QNWSP4LSN5GESJA3VZ4B727DBA/graph.json","events_json":"https://pith.science/api/pith-number/QNWSP4LSN5GESJA3VZ4B727DBA/events.json","paper":"https://pith.science/paper/QNWSP4LS"},"agent_actions":{"view_html":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA","download_json":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA.json","view_paper":"https://pith.science/paper/QNWSP4LS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2504.21813&json=true","fetch_graph":"https://pith.science/api/pith-number/QNWSP4LSN5GESJA3VZ4B727DBA/graph.json","fetch_events":"https://pith.science/api/pith-number/QNWSP4LSN5GESJA3VZ4B727DBA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA/action/storage_attestation","attest_author":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA/action/author_attestation","sign_citation":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA/action/citation_signature","submit_replication":"https://pith.science/pith/QNWSP4LSN5GESJA3VZ4B727DBA/action/replication_record"}},"created_at":"2026-07-05T10:56:29.777551+00:00","updated_at":"2026-07-05T10:56:29.777551+00:00"}