{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:LTYXYFGL7WV3IWXVYEOKWGB5XC","short_pith_number":"pith:LTYXYFGL","schema_version":"1.0","canonical_sha256":"5cf17c14cbfdabb45af5c11cab183db8a138c4589b38f9fa1f129f3b5580bcd9","source":{"kind":"arxiv","id":"1712.08617","version":2},"attestation_state":"computed","paper":{"title":"Planck 2015 constraints on the non-flat $\\phi$CDM inflation model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Bharat Ratra, Junpei Ooba, Naoshi Sugiyama","submitted_at":"2017-12-04T07:13:32Z","abstract_excerpt":"We perform Markov chain Monte Carlo analyses to put constraints on the non-flat $\\phi$CDM inflation model using Planck 2015 cosmic microwave background (CMB) anisotropy data and baryon acoustic oscillation distance measurements. The $\\phi$CDM model is a consistent dynamical dark energy model in which the currently accelerating cosmological expansion is powered by a scalar field $\\phi$ slowly rolling down an inverse power-law potential energy density. We also use a physically consistent power spectrum for energy density inhomogeneities in this non-flat model. We find that, like the closed-$\\Lam"},"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":"1712.08617","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-12-04T07:13:32Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"b77b977e4ed3e421c51ae03acaa50fae5ac472c395454f335d009a464772dabf","abstract_canon_sha256":"a73d4c83f6c5ba9b963aed6a49ec7e3b3b2a8dec86474b608b9f094363616662"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:02:35.869024Z","signature_b64":"0UZ0282/pRB1WjwnZnETJXQuIO7I13k5hdfdzghaEi1BtpKQla9ZvGutwJYuFsK+iEzY4JwVF0tp9h7l3qFNAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5cf17c14cbfdabb45af5c11cab183db8a138c4589b38f9fa1f129f3b5580bcd9","last_reissued_at":"2026-05-18T00:02:35.868384Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:02:35.868384Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Planck 2015 constraints on the non-flat $\\phi$CDM inflation model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Bharat Ratra, Junpei Ooba, Naoshi Sugiyama","submitted_at":"2017-12-04T07:13:32Z","abstract_excerpt":"We perform Markov chain Monte Carlo analyses to put constraints on the non-flat $\\phi$CDM inflation model using Planck 2015 cosmic microwave background (CMB) anisotropy data and baryon acoustic oscillation distance measurements. The $\\phi$CDM model is a consistent dynamical dark energy model in which the currently accelerating cosmological expansion is powered by a scalar field $\\phi$ slowly rolling down an inverse power-law potential energy density. We also use a physically consistent power spectrum for energy density inhomogeneities in this non-flat model. We find that, like the closed-$\\Lam"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1712.08617","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":""},"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":"1712.08617","created_at":"2026-05-18T00:02:35.868475+00:00"},{"alias_kind":"arxiv_version","alias_value":"1712.08617v2","created_at":"2026-05-18T00:02:35.868475+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1712.08617","created_at":"2026-05-18T00:02:35.868475+00:00"},{"alias_kind":"pith_short_12","alias_value":"LTYXYFGL7WV3","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_16","alias_value":"LTYXYFGL7WV3IWXV","created_at":"2026-05-18T12:31:28.150371+00:00"},{"alias_kind":"pith_short_8","alias_value":"LTYXYFGL","created_at":"2026-05-18T12:31:28.150371+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":8,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC","json":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC.json","graph_json":"https://pith.science/api/pith-number/LTYXYFGL7WV3IWXVYEOKWGB5XC/graph.json","events_json":"https://pith.science/api/pith-number/LTYXYFGL7WV3IWXVYEOKWGB5XC/events.json","paper":"https://pith.science/paper/LTYXYFGL"},"agent_actions":{"view_html":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC","download_json":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC.json","view_paper":"https://pith.science/paper/LTYXYFGL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1712.08617&json=true","fetch_graph":"https://pith.science/api/pith-number/LTYXYFGL7WV3IWXVYEOKWGB5XC/graph.json","fetch_events":"https://pith.science/api/pith-number/LTYXYFGL7WV3IWXVYEOKWGB5XC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC/action/storage_attestation","attest_author":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC/action/author_attestation","sign_citation":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC/action/citation_signature","submit_replication":"https://pith.science/pith/LTYXYFGL7WV3IWXVYEOKWGB5XC/action/replication_record"}},"created_at":"2026-05-18T00:02:35.868475+00:00","updated_at":"2026-05-18T00:02:35.868475+00:00"}