{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:MWXF5N277FZNIB3DUOIXUO4DCQ","short_pith_number":"pith:MWXF5N27","schema_version":"1.0","canonical_sha256":"65ae5eb75ff972d40763a3917a3b83140c9ce593460b6eee45e89644022e962a","source":{"kind":"arxiv","id":"astro-ph/9908023","version":1},"attestation_state":"computed","paper":{"title":"Coupled Quintessence","license":"","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph","authors_text":"Luca Amendola (Osservatorio Astronomico di Roma)","submitted_at":"1999-08-03T16:13:46Z","abstract_excerpt":"A new component of the cosmic medium, a light scalar field or ''quintessence '', has been proposed recently to explain cosmic acceleration with a dynamical cosmological constant. Such a field is expected to be coupled explicitely to ordinary matter, unless some unknown symmetry prevents it. I investigate the cosmological consequences of such a coupled quintessence (CQ) model, assuming an exponential potential and a linear coupling. This model is conformally equivalent to Brans-Dicke Lagrangians with power-law potential. I evaluate the density perturbations on the cosmic microwave background an"},"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":"astro-ph/9908023","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-08-03T16:13:46Z","cross_cats_sorted":["hep-th"],"title_canon_sha256":"4916167135378ae9f00a4855acb577231eca034683c8d55de8d4d77977a7d124","abstract_canon_sha256":"54985086021a430875686b11f647db3c16ef110e7d5b6afd61c4a1758e7af29a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:22:06.415895Z","signature_b64":"7ikA1hBAvQ2otzF2l1vC4/aAXAnFe4PCRe4BWLjFuFMVrx6UPUupnx2FvmSs0fnmTSgjZdyLMBVK/TcuKrRvCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"65ae5eb75ff972d40763a3917a3b83140c9ce593460b6eee45e89644022e962a","last_reissued_at":"2026-07-04T17:22:06.415425Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:22:06.415425Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Coupled Quintessence","license":"","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph","authors_text":"Luca Amendola (Osservatorio Astronomico di Roma)","submitted_at":"1999-08-03T16:13:46Z","abstract_excerpt":"A new component of the cosmic medium, a light scalar field or ''quintessence '', has been proposed recently to explain cosmic acceleration with a dynamical cosmological constant. Such a field is expected to be coupled explicitely to ordinary matter, unless some unknown symmetry prevents it. I investigate the cosmological consequences of such a coupled quintessence (CQ) model, assuming an exponential potential and a linear coupling. This model is conformally equivalent to Brans-Dicke Lagrangians with power-law potential. I evaluate the density perturbations on the cosmic microwave background an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9908023","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/astro-ph/9908023/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":"astro-ph/9908023","created_at":"2026-07-04T17:22:06.415484+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9908023v1","created_at":"2026-07-04T17:22:06.415484+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9908023","created_at":"2026-07-04T17:22:06.415484+00:00"},{"alias_kind":"pith_short_12","alias_value":"MWXF5N277FZN","created_at":"2026-07-04T17:22:06.415484+00:00"},{"alias_kind":"pith_short_16","alias_value":"MWXF5N277FZNIB3D","created_at":"2026-07-04T17:22:06.415484+00:00"},{"alias_kind":"pith_short_8","alias_value":"MWXF5N27","created_at":"2026-07-04T17:22:06.415484+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":29,"internal_anchor_count":21,"sample":[{"citing_arxiv_id":"2607.07777","citing_title":"The Status of Single Scalar Field Dark Energy","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"2606.11368","citing_title":"Non-linear Structure Formation in Planck+DESI Favoured Interacting Dark Energy Cosmologies","ref_index":23,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05539","citing_title":"Dissipative Cosmology and the Nature of Dark Energy: Insights from Bulk Viscosity with DESI DR2 observations","ref_index":58,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05005","citing_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","ref_index":9,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05133","citing_title":"CMB Bounds on Primordial Black Holes via Radiation Capture","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2606.04886","citing_title":"Dissipative Dark Energy can explain the DESI phantom crossing","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2606.01360","citing_title":"A short review on Quintom dark energy theory","ref_index":107,"is_internal_anchor":true},{"citing_arxiv_id":"2605.30926","citing_title":"Matter influence on large-scale scalar dynamics","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28288","citing_title":"Generalizing the interacting dilatonic ghost condensate as a dark energy model","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28246","citing_title":"The cosmology of long range Yukawa interactions in general backgrounds","ref_index":63,"is_internal_anchor":true},{"citing_arxiv_id":"2605.10476","citing_title":"Breaking Free from the Swampland of Impossible Universes through the DESI Portal","ref_index":266,"is_internal_anchor":true},{"citing_arxiv_id":"2605.25671","citing_title":"Scalarization of dark matter stars","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2605.27301","citing_title":"Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2605.27357","citing_title":"Gaussian Process Reconstruction of Cosmological Parameters with Gravitational Wave Sirens using Machine Learning","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2606.21826","citing_title":"Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\\Lambda$CDM Interpretations, and Tensions","ref_index":73,"is_internal_anchor":true},{"citing_arxiv_id":"2604.25373","citing_title":"Generalizing the CPL Parametrization through Dark Sector Interaction","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2605.16220","citing_title":"Non-minimal fluid Lagrangian couplings","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2508.01759","citing_title":"Resolving the Planck-DESI tension by nonminimally coupled quintessence","ref_index":59,"is_internal_anchor":true},{"citing_arxiv_id":"2511.16244","citing_title":"Constraining interacting dark energy models with black hole superradiance","ref_index":83,"is_internal_anchor":true},{"citing_arxiv_id":"2603.12321","citing_title":"Phenomenology of an Open Effective Field Theory of Dark Energy","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2503.14743","citing_title":"Extended Dark Energy analysis using DESI DR2 BAO measurements","ref_index":194,"is_internal_anchor":true},{"citing_arxiv_id":"2604.02204","citing_title":"Non-minimally coupled quintessence with sign-switching interaction","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25373","citing_title":"Generalizing the CPL Parametrization through Dark Sector Interaction","ref_index":33,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21770","citing_title":"Accelerating scaling solutions from dark matter particle creation","ref_index":82,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08530","citing_title":"Disentangling cosmic distance tensions with early and late dark energy","ref_index":25,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ","json":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ.json","graph_json":"https://pith.science/api/pith-number/MWXF5N277FZNIB3DUOIXUO4DCQ/graph.json","events_json":"https://pith.science/api/pith-number/MWXF5N277FZNIB3DUOIXUO4DCQ/events.json","paper":"https://pith.science/paper/MWXF5N27"},"agent_actions":{"view_html":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ","download_json":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ.json","view_paper":"https://pith.science/paper/MWXF5N27","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9908023&json=true","fetch_graph":"https://pith.science/api/pith-number/MWXF5N277FZNIB3DUOIXUO4DCQ/graph.json","fetch_events":"https://pith.science/api/pith-number/MWXF5N277FZNIB3DUOIXUO4DCQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ/action/storage_attestation","attest_author":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ/action/author_attestation","sign_citation":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ/action/citation_signature","submit_replication":"https://pith.science/pith/MWXF5N277FZNIB3DUOIXUO4DCQ/action/replication_record"}},"created_at":"2026-07-04T17:22:06.415484+00:00","updated_at":"2026-07-04T17:22:06.415484+00:00"}