{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:DI7ZKVVIH44KQDJZBGZNWVAYYA","short_pith_number":"pith:DI7ZKVVI","schema_version":"1.0","canonical_sha256":"1a3f9556a83f38a80d3909b2db5418c031f75f05b18eec01936005f2b7c699af","source":{"kind":"arxiv","id":"2308.05807","version":3},"attestation_state":"computed","paper":{"title":"Constraints on interacting dark energy revisited: implications for the Hubble tension","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Elcio Abdalla, Filipe B. Abdalla, Gabriel A. Hoerning, Luiza O. Ponte, Raphael P. Rolim, Ricardo G. Landim","submitted_at":"2023-08-10T18:03:39Z","abstract_excerpt":"We revisit a class of coupled dark energy models where dark energy interacts with dark matter via phenomenological energy exchange terms. We include the perturbation of the Hubble rate in the interaction term, which was absent in previous works. We also consider more recent data sets such as cosmic microwave background (CMB) anisotropies from \\text{Planck} 2018, type I-a supernovae (SNIa) measurements from Pantheon+ and data from baryon acoustic oscillations (BAO), and redshift space distortions (RSD). One of the models presents a strong incompatibility when different cosmological datasets are"},"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":"2308.05807","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-08-10T18:03:39Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"8e7e33347db6ad9ac0731d07c1856d9984a5c3e7fa6d03111b396a87e11d4c91","abstract_canon_sha256":"287e2761227faaa48c04e5ab7948d5868819527e6b8485588dee564d98044194"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:37:06.861769Z","signature_b64":"Prn/xeExdDoptWi/lByufbSUZ4CpORzrr2OyZRn2I9fic6ERdRikrdx7RvMPXuPID2CROCHjmI7oqY35/dY6AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1a3f9556a83f38a80d3909b2db5418c031f75f05b18eec01936005f2b7c699af","last_reissued_at":"2026-07-05T11:37:06.861221Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:37:06.861221Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraints on interacting dark energy revisited: implications for the Hubble tension","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Elcio Abdalla, Filipe B. Abdalla, Gabriel A. Hoerning, Luiza O. Ponte, Raphael P. Rolim, Ricardo G. Landim","submitted_at":"2023-08-10T18:03:39Z","abstract_excerpt":"We revisit a class of coupled dark energy models where dark energy interacts with dark matter via phenomenological energy exchange terms. We include the perturbation of the Hubble rate in the interaction term, which was absent in previous works. We also consider more recent data sets such as cosmic microwave background (CMB) anisotropies from \\text{Planck} 2018, type I-a supernovae (SNIa) measurements from Pantheon+ and data from baryon acoustic oscillations (BAO), and redshift space distortions (RSD). One of the models presents a strong incompatibility when different cosmological datasets are"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2308.05807","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/2308.05807/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":"2308.05807","created_at":"2026-07-05T11:37:06.861281+00:00"},{"alias_kind":"arxiv_version","alias_value":"2308.05807v3","created_at":"2026-07-05T11:37:06.861281+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2308.05807","created_at":"2026-07-05T11:37:06.861281+00:00"},{"alias_kind":"pith_short_12","alias_value":"DI7ZKVVIH44K","created_at":"2026-07-05T11:37:06.861281+00:00"},{"alias_kind":"pith_short_16","alias_value":"DI7ZKVVIH44KQDJZ","created_at":"2026-07-05T11:37:06.861281+00:00"},{"alias_kind":"pith_short_8","alias_value":"DI7ZKVVI","created_at":"2026-07-05T11:37:06.861281+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.11368","citing_title":"Non-linear Structure Formation in Planck+DESI Favoured Interacting Dark Energy Cosmologies","ref_index":59,"is_internal_anchor":false},{"citing_arxiv_id":"2606.06495","citing_title":"What it takes to solve the Hubble tension through Modifications of Cosmological Recombination II: in light of ACT DR6 and DESI DR2","ref_index":76,"is_internal_anchor":false},{"citing_arxiv_id":"2605.26116","citing_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","ref_index":189,"is_internal_anchor":false},{"citing_arxiv_id":"2605.20060","citing_title":"Interacting Dark Sector field theory with phantom crossing","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2601.14222","citing_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","ref_index":99,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA","json":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA.json","graph_json":"https://pith.science/api/pith-number/DI7ZKVVIH44KQDJZBGZNWVAYYA/graph.json","events_json":"https://pith.science/api/pith-number/DI7ZKVVIH44KQDJZBGZNWVAYYA/events.json","paper":"https://pith.science/paper/DI7ZKVVI"},"agent_actions":{"view_html":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA","download_json":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA.json","view_paper":"https://pith.science/paper/DI7ZKVVI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2308.05807&json=true","fetch_graph":"https://pith.science/api/pith-number/DI7ZKVVIH44KQDJZBGZNWVAYYA/graph.json","fetch_events":"https://pith.science/api/pith-number/DI7ZKVVIH44KQDJZBGZNWVAYYA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA/action/storage_attestation","attest_author":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA/action/author_attestation","sign_citation":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA/action/citation_signature","submit_replication":"https://pith.science/pith/DI7ZKVVIH44KQDJZBGZNWVAYYA/action/replication_record"}},"created_at":"2026-07-05T11:37:06.861281+00:00","updated_at":"2026-07-05T11:37:06.861281+00:00"}