{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:KCF5P75NKJOYYNVHVGZ7RE53KI","short_pith_number":"pith:KCF5P75N","schema_version":"1.0","canonical_sha256":"508bd7ffad525d8c36a7a9b3f893bb523dc10859fff459efaf426fdb6c1a76fc","source":{"kind":"arxiv","id":"2406.02688","version":1},"attestation_state":"computed","paper":{"title":"Holographic motivations and observational evidence for decreasing dark energy","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Chris Waddell, Mark Van Raamsdonk","submitted_at":"2024-06-04T18:01:17Z","abstract_excerpt":"Negative lambda gravitational effective field theories dual to holographic CFTs have potentially realistic cosmological solutions. Generic cosmological solutions of these effective field theories have scalar field evolution that can lead to a period of accelerated expansion when the scalar field is at positive values of its potential (Fig. 1). If such a model describes our universe, significant evolution of dark energy is expected over a Hubble time as the scalar descends from positive to negative values of its potential towards the AdS extremum. Our recent observational study 2305.04946 based"},"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":"2406.02688","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-th","submitted_at":"2024-06-04T18:01:17Z","cross_cats_sorted":["astro-ph.CO","gr-qc"],"title_canon_sha256":"a2ca0afd5d39aa2a43d8433de7620d0890019cce17d6731ed3905261510b76ee","abstract_canon_sha256":"d355d52c9b70ed586203838f611d0666dea8c7410df52d6ca0f6ca163e5f05c4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:27:28.801726Z","signature_b64":"Auo2nlV+GJozIdiQJwXRS4eVexOGXyYrCPlvbBftWfoKTguSLhJmA4Wv14NggHZ8ft5DeKeD1/SdXWQiPxuCBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"508bd7ffad525d8c36a7a9b3f893bb523dc10859fff459efaf426fdb6c1a76fc","last_reissued_at":"2026-07-05T08:27:28.801252Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:27:28.801252Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Holographic motivations and observational evidence for decreasing dark energy","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Chris Waddell, Mark Van Raamsdonk","submitted_at":"2024-06-04T18:01:17Z","abstract_excerpt":"Negative lambda gravitational effective field theories dual to holographic CFTs have potentially realistic cosmological solutions. Generic cosmological solutions of these effective field theories have scalar field evolution that can lead to a period of accelerated expansion when the scalar field is at positive values of its potential (Fig. 1). If such a model describes our universe, significant evolution of dark energy is expected over a Hubble time as the scalar descends from positive to negative values of its potential towards the AdS extremum. Our recent observational study 2305.04946 based"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2406.02688","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/2406.02688/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":"2406.02688","created_at":"2026-07-05T08:27:28.801308+00:00"},{"alias_kind":"arxiv_version","alias_value":"2406.02688v1","created_at":"2026-07-05T08:27:28.801308+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2406.02688","created_at":"2026-07-05T08:27:28.801308+00:00"},{"alias_kind":"pith_short_12","alias_value":"KCF5P75NKJOY","created_at":"2026-07-05T08:27:28.801308+00:00"},{"alias_kind":"pith_short_16","alias_value":"KCF5P75NKJOYYNVH","created_at":"2026-07-05T08:27:28.801308+00:00"},{"alias_kind":"pith_short_8","alias_value":"KCF5P75N","created_at":"2026-07-05T08:27:28.801308+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.03756","citing_title":"Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?","ref_index":19,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI","json":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI.json","graph_json":"https://pith.science/api/pith-number/KCF5P75NKJOYYNVHVGZ7RE53KI/graph.json","events_json":"https://pith.science/api/pith-number/KCF5P75NKJOYYNVHVGZ7RE53KI/events.json","paper":"https://pith.science/paper/KCF5P75N"},"agent_actions":{"view_html":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI","download_json":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI.json","view_paper":"https://pith.science/paper/KCF5P75N","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2406.02688&json=true","fetch_graph":"https://pith.science/api/pith-number/KCF5P75NKJOYYNVHVGZ7RE53KI/graph.json","fetch_events":"https://pith.science/api/pith-number/KCF5P75NKJOYYNVHVGZ7RE53KI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI/action/storage_attestation","attest_author":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI/action/author_attestation","sign_citation":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI/action/citation_signature","submit_replication":"https://pith.science/pith/KCF5P75NKJOYYNVHVGZ7RE53KI/action/replication_record"}},"created_at":"2026-07-05T08:27:28.801308+00:00","updated_at":"2026-07-05T08:27:28.801308+00:00"}