{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:7AZZVQOJPGLCBHHT3V2LNH4NZR","short_pith_number":"pith:7AZZVQOJ","schema_version":"1.0","canonical_sha256":"f8339ac1c97996209cf3dd74b69f8dcc4dd755674a5b27f6b86df8e9a2390475","source":{"kind":"arxiv","id":"2408.14628","version":2},"attestation_state":"computed","paper":{"title":"Investigating Late-Time Dark Energy and Massive Neutrinos in Light of DESI Y1 BAO","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Diogo H. F. de Souza, Jo\\~ao Rebou\\c{c}as, Kunhao Zhong, Rogerio Rosenfeld, Vivian Miranda","submitted_at":"2024-08-26T20:45:51Z","abstract_excerpt":"Baryonic Acoustic Oscillation (BAO) data from the Dark Energy Spectroscopic Instrument (DESI), in combination with Cosmic Microwave Background (CMB) data and Type Ia Supernovae (SN) luminosity distances, suggests a dynamical evolution of the dark energy equation of state with a phantom phase ($w < -1$) in the past when the so-called $w_0w_a$ parametrization $w(a) = w_0 + w_a(1-a)$ is assumed. In this work, we investigate more general dark energy models that also allow a phantom equation of state. We consider three cases: an equation of state with a transition feature, a model-agnostic equation"},"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":"2408.14628","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-08-26T20:45:51Z","cross_cats_sorted":[],"title_canon_sha256":"efb74bf1ff67e5b8235b4b7a86580c8a6936fdac5b7111e9493314d3ac7ad756","abstract_canon_sha256":"f4cb0d2f08ca016335ad139349d86a14c8746ef1bd3117bfe57c34e9ec378473"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:07:43.861373Z","signature_b64":"bPzEriqQ9lz3M8NzNT/a/A5jLr/z3cDSEAyidd+Xa6IxaCb9YIFl9VwK1NTLy+nt1wUcwOaA+QJM/8mRQ1vzBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f8339ac1c97996209cf3dd74b69f8dcc4dd755674a5b27f6b86df8e9a2390475","last_reissued_at":"2026-07-05T10:07:43.860920Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:07:43.860920Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Investigating Late-Time Dark Energy and Massive Neutrinos in Light of DESI Y1 BAO","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Diogo H. F. de Souza, Jo\\~ao Rebou\\c{c}as, Kunhao Zhong, Rogerio Rosenfeld, Vivian Miranda","submitted_at":"2024-08-26T20:45:51Z","abstract_excerpt":"Baryonic Acoustic Oscillation (BAO) data from the Dark Energy Spectroscopic Instrument (DESI), in combination with Cosmic Microwave Background (CMB) data and Type Ia Supernovae (SN) luminosity distances, suggests a dynamical evolution of the dark energy equation of state with a phantom phase ($w < -1$) in the past when the so-called $w_0w_a$ parametrization $w(a) = w_0 + w_a(1-a)$ is assumed. In this work, we investigate more general dark energy models that also allow a phantom equation of state. We consider three cases: an equation of state with a transition feature, a model-agnostic equation"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2408.14628","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/2408.14628/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":"2408.14628","created_at":"2026-07-05T10:07:43.860976+00:00"},{"alias_kind":"arxiv_version","alias_value":"2408.14628v2","created_at":"2026-07-05T10:07:43.860976+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2408.14628","created_at":"2026-07-05T10:07:43.860976+00:00"},{"alias_kind":"pith_short_12","alias_value":"7AZZVQOJPGLC","created_at":"2026-07-05T10:07:43.860976+00:00"},{"alias_kind":"pith_short_16","alias_value":"7AZZVQOJPGLCBHHT","created_at":"2026-07-05T10:07:43.860976+00:00"},{"alias_kind":"pith_short_8","alias_value":"7AZZVQOJ","created_at":"2026-07-05T10:07:43.860976+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":13,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06147","citing_title":"Imprint of swampland-inspired coupled early dark energy","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19090","citing_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","ref_index":73,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05853","citing_title":"Reconstructing dark energy with fewer assumptions","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2606.05005","citing_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","ref_index":28,"is_internal_anchor":false},{"citing_arxiv_id":"2607.01226","citing_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","ref_index":131,"is_internal_anchor":false},{"citing_arxiv_id":"2606.01360","citing_title":"A short review on Quintom dark energy theory","ref_index":36,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31324","citing_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","ref_index":80,"is_internal_anchor":false},{"citing_arxiv_id":"2606.00411","citing_title":"The sound of dynamical dark energy and modified gravity","ref_index":36,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21456","citing_title":"Negative neutrino mass or negative dark energy?","ref_index":133,"is_internal_anchor":false},{"citing_arxiv_id":"2505.24732","citing_title":"The Quintom theory of dark energy after DESI DR2","ref_index":106,"is_internal_anchor":false},{"citing_arxiv_id":"2409.13022","citing_title":"Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble","ref_index":53,"is_internal_anchor":false},{"citing_arxiv_id":"2510.14888","citing_title":"Modeling nonlinear scales for dynamical dark energy cosmologies with COLA","ref_index":65,"is_internal_anchor":false},{"citing_arxiv_id":"2503.14743","citing_title":"Extended Dark Energy analysis using DESI DR2 BAO measurements","ref_index":133,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR","json":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR.json","graph_json":"https://pith.science/api/pith-number/7AZZVQOJPGLCBHHT3V2LNH4NZR/graph.json","events_json":"https://pith.science/api/pith-number/7AZZVQOJPGLCBHHT3V2LNH4NZR/events.json","paper":"https://pith.science/paper/7AZZVQOJ"},"agent_actions":{"view_html":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR","download_json":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR.json","view_paper":"https://pith.science/paper/7AZZVQOJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2408.14628&json=true","fetch_graph":"https://pith.science/api/pith-number/7AZZVQOJPGLCBHHT3V2LNH4NZR/graph.json","fetch_events":"https://pith.science/api/pith-number/7AZZVQOJPGLCBHHT3V2LNH4NZR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR/action/storage_attestation","attest_author":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR/action/author_attestation","sign_citation":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR/action/citation_signature","submit_replication":"https://pith.science/pith/7AZZVQOJPGLCBHHT3V2LNH4NZR/action/replication_record"}},"created_at":"2026-07-05T10:07:43.860976+00:00","updated_at":"2026-07-05T10:07:43.860976+00:00"}