{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:PCAYVEBH4GIZOMTU57C7EOQLGU","short_pith_number":"pith:PCAYVEBH","schema_version":"1.0","canonical_sha256":"78818a9027e191973274efc5f23a0b35376a9a2dd91548af7276745d2a8be2f5","source":{"kind":"arxiv","id":"2412.04430","version":2},"attestation_state":"computed","paper":{"title":"Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in $\\Omega_m$ and $H_0$ Across Cosmological Probes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Chihway Chang, Dillon Brout, Maria Vincenzi, Tanvi Karwal, Vivian Miranda, Xianzhe TZ Tang","submitted_at":"2024-12-05T18:52:01Z","abstract_excerpt":"Recent results from Type Ia Supernovae (SNe), baryon acoustic oscillations (BAO), and the cosmic microwave background (CMB) indicate 1) potentially discrepant measurements of the matter density $\\Omega_m$ and Hubble constant $ H_0 $ in $\\Lambda$CDM model when analyzed individually, and 2) hints of dynamical dark energy in a $w_0w_a$CDM model when data are combined in a joint analysis. We examine whether underlying dynamical dark energy cosmologies favored by data would result in biases in $\\Omega_m$ and $ H_0 $ for each probe when analyzed individually under $\\Lambda$CDM. We generate mock data"},"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":"2412.04430","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-12-05T18:52:01Z","cross_cats_sorted":[],"title_canon_sha256":"1d2183dcb7327e82d0c35e4a68faeb3960b3731a508d2fa65797bfcd9f895b9b","abstract_canon_sha256":"2ea6ab669e81969374b506212326d0634b75f6b38caed3e3cf723919853ae7ab"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:37:39.558137Z","signature_b64":"bMhN+0P6NauxvasI0lZoEz6PlV8RL3V0l/XarU8g4DBcTJuQKa+I9eJCIS/N0U04Aubx8Jk0VMkyRvK9YR+2Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"78818a9027e191973274efc5f23a0b35376a9a2dd91548af7276745d2a8be2f5","last_reissued_at":"2026-07-05T10:37:39.553814Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:37:39.553814Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in $\\Omega_m$ and $H_0$ Across Cosmological Probes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Chihway Chang, Dillon Brout, Maria Vincenzi, Tanvi Karwal, Vivian Miranda, Xianzhe TZ Tang","submitted_at":"2024-12-05T18:52:01Z","abstract_excerpt":"Recent results from Type Ia Supernovae (SNe), baryon acoustic oscillations (BAO), and the cosmic microwave background (CMB) indicate 1) potentially discrepant measurements of the matter density $\\Omega_m$ and Hubble constant $ H_0 $ in $\\Lambda$CDM model when analyzed individually, and 2) hints of dynamical dark energy in a $w_0w_a$CDM model when data are combined in a joint analysis. We examine whether underlying dynamical dark energy cosmologies favored by data would result in biases in $\\Omega_m$ and $ H_0 $ for each probe when analyzed individually under $\\Lambda$CDM. We generate mock data"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2412.04430","kind":"arxiv","version":2},"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/2412.04430/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":"2412.04430","created_at":"2026-07-05T10:37:39.557412+00:00"},{"alias_kind":"arxiv_version","alias_value":"2412.04430v2","created_at":"2026-07-05T10:37:39.557412+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2412.04430","created_at":"2026-07-05T10:37:39.557412+00:00"},{"alias_kind":"pith_short_12","alias_value":"PCAYVEBH4GIZ","created_at":"2026-07-05T10:37:39.557412+00:00"},{"alias_kind":"pith_short_16","alias_value":"PCAYVEBH4GIZOMTU","created_at":"2026-07-05T10:37:39.557412+00:00"},{"alias_kind":"pith_short_8","alias_value":"PCAYVEBH","created_at":"2026-07-05T10:37:39.557412+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.19090","citing_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","ref_index":134,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05853","citing_title":"Reconstructing dark energy with fewer assumptions","ref_index":81,"is_internal_anchor":false},{"citing_arxiv_id":"2506.23290","citing_title":"Type II Seesaw Leptogenesis in a Majoron background","ref_index":104,"is_internal_anchor":false},{"citing_arxiv_id":"2503.14744","citing_title":"Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape","ref_index":183,"is_internal_anchor":false},{"citing_arxiv_id":"2503.14738","citing_title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","ref_index":132,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU","json":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU.json","graph_json":"https://pith.science/api/pith-number/PCAYVEBH4GIZOMTU57C7EOQLGU/graph.json","events_json":"https://pith.science/api/pith-number/PCAYVEBH4GIZOMTU57C7EOQLGU/events.json","paper":"https://pith.science/paper/PCAYVEBH"},"agent_actions":{"view_html":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU","download_json":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU.json","view_paper":"https://pith.science/paper/PCAYVEBH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2412.04430&json=true","fetch_graph":"https://pith.science/api/pith-number/PCAYVEBH4GIZOMTU57C7EOQLGU/graph.json","fetch_events":"https://pith.science/api/pith-number/PCAYVEBH4GIZOMTU57C7EOQLGU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU/action/storage_attestation","attest_author":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU/action/author_attestation","sign_citation":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU/action/citation_signature","submit_replication":"https://pith.science/pith/PCAYVEBH4GIZOMTU57C7EOQLGU/action/replication_record"}},"created_at":"2026-07-05T10:37:39.557412+00:00","updated_at":"2026-07-05T10:37:39.557412+00:00"}